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The R.A.P. Project (Reviews of Astro-Ph)

Neitronnye zvezdy

Vypusk 202. 17-31 dekabrya 2008

arxiv:0812.3018 Magnito-teplovaya evolyuciya neitronnyh zvezd (Magneto-thermal evolution of neutron stars)
Authors: J.A. Pons et al.
Comments: 10 pages, accepted for publication in A&A

Neitronnye zvezdy - evolyucioniruyushie ob'ekty. Vo-pervyh, esli vy rassmatrivaem odinochnye neitronnye zvezdy, oni zamedlyayut svoe vrashenie. Temp zamedleniya vrasheniya zavisit ot magnitnogo polya, kotoroe samo mozhet izmenyat'sya. Svyazano eto s tem, chto pole porozhdaetsya tokami, a toki dolzhny zatuhat'. Sootvetstvenno, govoryat o "magnito-vrashatel'noi evolyucii". Krome togo, neitronnye zvezdy rozhdayutsya goryachimi, a potom potihon'ku ostyvayut za schet izlucheniya neitrino iz ih nedr i fotonov s poverhnosti. Sootvetstvenno, govoryat o teplovoi evolyucii. No, esli toki sil'ny i zatuhayut dovol'no bystro, to ih energiya poidet na nagrev kory neitronnoi zvezdy. Sootvetstvenno, voznikaet svyaz' mezhdu magnitnoi i teplovoi evolyuciei.

Jose Pons i ego kollegi uzhe neskol'ko let sovershenstvuyut model' zatuhaniya magnitnogo polya i raschety progreva kory. Sushestvennaya cherta predstavlyaemoi modeli sostoit v tom, chto sil'nye polya zatuhayut bystree i zametnee. V itoge, po nablyudeniyam obychnyh radiopul'sarov my ne dolzhny videt' sledov raspada, a vot dlya magnitarov zatuhanie polya kraine vazhno.


arxiv:0812.4248 Vybros veshestva pri sliyaniyah strannyh zvezd i nablyudatel'nye prilozheniya (Mass Ejection by Strange Star Mergers and Observational Implications)
Authors: A. Bauswein et al.
Comments: 5 pages, 2 eps figures; submitted to Phys. Rev. Lett

Strapel'ki - kapel'ki strannogo veshestva - dolzhny vybrasyvat'sya v mezhzvezdnuyu sredu pri sliyaniyah kompaktnyh ob'ektov so strannoi materiei vnutri. Dlya rascheta nablyudaemosti strapelek (naprimer, v kosmicheskih luchah) neobhodimo rasschitat' temp ih vbrosa. Chto avtory i delayut.

Razumeetsya, rezul'taty ochen' model'no zavisimy. Sushestvenno, chto pri bol'shom znachenii t.n. bag constant (80 MeV/fm3) vybrasyvaetsya malo. Sootvetstvenno, v takom sluchae i strapelek v mezhzvezdnom prostranstve budet malo, znachit, obychnye neitronnye zvezdy redko budut ih zahvatyvat', prevrashayas' v strannye. Avtory polagayut, chto v takom sluchae obnaruzhenie neitronnyh zvezd v toi oblasti parametrov, gde mogli by sushestvovat' kvarkovye, vovse ne zakryvaet gipotezu o "kvarkovosti" chasti kompaktnyh ob'ektov. Ravno ne zakroet etu gipotezu, po mneniyu avtorov, i nulevoi rezul'tat AMS-02 (polagayut, chto etot kosmicheskii eksperiment smozhet registrirovat' strapel'ki) ne zakroet samu gipotezu o strannom veshestve.


Vypusk 201. 01-16 dekabrya 2008

arxiv:0812.0014 XMM-Newton obnaruzhil 2.6-sekundnye pul'sacii v istochnike myagkih povtoryayushihsya gamma-vspleskov SGR 1627-41 (XMM-Newton discovery of 2.6 s pulsations in the soft gamma-ray repeater SGR 1627-41)
Authors: P. Esposito et al.
Comments: 4 pages, accepted for publiaction in ApJ Letters

SGR 1627-41 byl edinstvennym istochnikom etogo tipa, dlya kotorogo ne bylo supernadezhnyh izmerenii perioda. Okolo 10 let nazad byla publikaciya, v kotoroi govorilos' o vozmozhnom periode okolo 6.4 sekund, no podtverzhdenii ne bylo. V etoi stat'e avtory pishut o nadezhnom obnaruzhenii pul'sacii s periodom 2.6 sekundy.

Nablyudeniya provodilis' na sputnike XMM-Newton posle togo, kak istochnik opyat' voshel v polosu aktivnosti v mae 2008 goda. Poisk pul'sacii v arhivnyh dannyh ne dal rezul'tata.


!!!Vypusk 200!!!. 14-30 noyabrya 2008

arxiv:0811.2027 PSR J1753-2240: umerenno raskruchennyi pul'sar v ekscentrichnoi dvoinoi sisteme (PSR J1753-2240: a mildly recycled pulsar in an eccentric binary system)
Authors: M.J. Keith et al.
Comments: 6 pages, accepted for publication in MNRAS

Otkryt radiopul'sar, kotoryi mozhet okazat'sya interesnoi sistemoi, sostoyashei iz dvuh neitronnyh zvezd.

Pul'sar imeet period 95 millisekund i bol'shoi harakteristicheskii vozrast (milliard let). Eto govorit o tom, chto on byl raskruchen akkreciei. Orbial'nyi period 13.6 dnei. Pro vtoroi komponent poka izvestno tol'ko to, chto on massivnee 0.5 mass Solnca. Esli eto belyi karlik ili obychnaya zvezda, to eto mozhno budet proverit' v blizhaishem budushem (prosto nado posmotret' teleskopom tipa Habbla, Keka ili VLT). Vpolne veroyatno, chto eto vtoraya neitronnaya zvezda. Togda svoistva etoi sistemy dovol'no neobychny, poskol'ku ekscentrisitet orbity sostavlyaet 0.3. Obychno dlya sistem iz dvuh neitronnyh zvezd s pul'sarom s periodom vrasheniya poryadka sta millisekund ozhidayut ekscentrisiteta 0.8. Nizkii ekscentrisitet novoi sistemy mozhet oznachat', chto vtoraya neitronnaya zvezda poluchila sushestvennyi kik (tolchok) pri vzryve sverhnovoi, kotoryi byl napravlen tak, chto skompensiroval ozhidaemyi bol'shoi ekscentrisitet. Ili zhe sbros massy pri vtorom vzryve byl anomal'no nizok.


arxiv:0811.3605 Kak bystro vrashayutsya novorozhdennye neitronnye zvezdy? (How rapidly do neutron stars spin at birth?)
Authors: Roberto Soria et al.
Comments: 3 pages

Avtory ispol'zuyut dovol'no ostroumnyi podhod. Oni analiziruyut dannye rentgenovskih nablyudenii molodyh ostatkov sverhnovyh v drugih galaktikah. Tochnee dazhe tak. Oni analiziruyut, chto uvideli na meste vzryva sverhnovoi spustya neskol'ko desyatkov let posle vspyshki (chashe vsego prosto nichego ne vidyat). Otsutstvie registracii energichnyh molodyh pul'sarov v podavlyayushem bol'shinstve sluchaev pozvolyaet postavit' ser'eznye predely na raspredelenie neitronnyh zvezd po nachal'nym periodam (pri izvestnom raspredelenii po polyam). V chastnosti, dolya neitronnyh zvezd s nachal'nym periodom menee 40 millisekund dolzhna byt' ochen' mala (v to vremya kak seichas ochen' chasto v kachestve nachal'nogo raspredeleniya ispol'zuyut predpolozhenie ob ochen' korotkih periodah).


arxiv:0811.3979 Rasstoyanie, massa i radius neitronnoi zvezdy v sisteme 4U 1608-52 (The distance, mass, and radius of the neutron star in 4U 1608-52)
Authors: Tolga Guver et la.
Comments: 27 pages, submitted to ApJ

4U 1608-52 - rentgenovskii barster. Dlya takih istochnikov, izuchaya ih vspyshki, mozhno srazu poluchit' dannye o rasstoyanii, masse i radiuse zvezdy. Avtory privodyat sleduyushie znacheniya. Rasstoyanie - 5.16+/-0.72 kpk. Massa 1.84+/-0.09 mass Solnca. Radius 9.83+/-1.24 km.

Sm. takzhe arxiv:0811.2939, gde obsuzhdaetsya vopros o nalichii giperonov v neitronnyh zvezdah. Avtory prihodyat k vyvodu, chto giperony tam est' vsegda. Eto sushestvenno dlya postroeniya modelei i sravneniya ih s dannymi po izmereniyu mass i radiusov neitronnyh zvezd.


arxiv:0811.4311 Rannyaya evolyuciya novorozhdennyh magnitarov s sil'nym magnitnym polem (Early evolution of newly born magnetars with a strong magnetic field)
Authors: S. Dall'Osso et al.
Comments: 19 pages, accepted for publication in MNRAS

Novorozhdennye magnitary - potencial'nye istochniki gravitacionnyh voln. Ih forma dovol'no sil'no iskazhena sil'nym magnitnym polem, a potomu oni budut izluchat' gravvolny. Avtory davno issleduyut etot vopros. Dannaya stta'ya - naibolee polnoe issledovanie v etom napravlenii. Avtory taki nadeyutsya, chto gravitacionno-volnovye detektory sleduyushego pokoleniya (advanced LIGO i dr.) taki smogut videt' vspleski, svyazannye s molodymi magnitarami iz skopleniya v Deve s tempom okolo odnogo v god.


Vypusk 199. 01-13 noyabrya 2008

arxiv:0811.0211 Poisk pul'sarov i ih taiming na SKA (Pulsar searches and timing with the SKA)
Authors: R. Smits et al.
Comments: 12 pages, 9 figures, accepted for publication in A&A

Odnoi iz zadach dlya sistemy radioteleskopov SKA budet poisk novyh pul'sarov. Prichem, rech' idet ne tol'ko i ne stol'ko o prostom uvelichenii chisla otkrytyh ob'ektov, ili ob obnaruzhenii pul'sarov v blizkih galaktikah, a ob otkrytii ekzoticheskih sistem. Naprimer, mozhno leleyat' mechtu o nobelevskoi premii za obnaruzhenie pary pul'sar plyus chernaya dyra, vidimoi pochti s rebra (t.e., chtoby pul'sar "prosvechival" okrestnosti chernoi dyry).

V stat'e detal'no razbiraetsya, kak SKA smozhet issledovat' radiopul'sary. Zamechu, odnako, chto okonchatel'nyi dizain sistemy eshe ne vybran, poetomu ocenki mogut slegka popolzti. Po suti, prodolzhaetsya bor'ba mezhdu pul'sarnoi i vnegalakticheskoi programmami, kotorye trebuyut raznogo dizaina sistemy. Sushestvenno, chto kogda SKA nachnet rabotu, to dlya issledovanii pul'sarov ogranicheniem mozhet stat' ob'em dannyh. Nuzhny budut ochen' moshnye vychislitel'nye sredstva dlya obrabotki nablyudenii. Po suti, planiruya programmy, uchenye ekstrapoliruyut rost vychislitel'noi moshnosti komp'yuterov i stoimosti hraneniya dannyh. Ispol'zuemye ocenki: v 2015 godu 10 Pflop budut stoit' 100 millionov dollarov. T.e., bez progressa v etoi oblasti spravitsya s budushimi nablyudeniyami budet neprosto.

Ozhidaetsya, chto SKA uvidit bolee 20 000 pul'sarov (iz nih 6000 - millisekundnye). Vsego v Galaktike okolo 30 000 normal'nyh pul'sarov i stol'ko zhe milisekundnyh, ch'i signaly popadayut na Zemlyu (napomnyu, chto izluchenie pul'sara skoncentrirovano v dostatochno uzkom konuse). Razumeetsya, nado uchest', chto iz dannoi tochki Zemli ne vse nebo dostupno dlya nablyudenii. Kstati, eti ocenki pozvolyayut rasschityvat' na desyatok sistem pul'sar plyus chernaya dyra, tak chto odna iz nih mozhet imet' ploskost' orbity vblizi lucha zreniya. Optimizaciya sistemy dlya pul'sarnyh issledovanii pozvolit neskol'ko uvelichit' eto chislo, no na moi vzglyad, maloveroyatno, chto eto budet sdelano v usherb vnegalakticheskim issledovaniyam.

Kstati, v Living Reviews in Relativity (kotorye v etom godu prazdnuyut desyatiletie, i "Troickii variant" napishet ob etom) poyavilsya apdeit obzora po dvoinym i millisekundnym pul'saram, kotoryi budet horoshim dopolneniem k dannoi stat'e po pul'saram na SKA.


Vypusk 198. 20-31 oktyabrya 2008

arxiv:0810.3562 Otkrytie kosmicheskim gamma-teleskopom Fermi pul'sara v molodom galakticheskom ostatke sverhnovoi STA 1 (The Fermi gamma-ray space telescope discovers the pulsar in the young galactic supernova-remnant CTA1)
Authors: The Fermi LAT collaboration: G. Kanbach et al.
Comments: 18 pages, publshed in Science Express

Period pul'sara 316 millisekund. Ranee tam byl izvesten gamma-istochnik (a takzhe rentgenovskii tochechnyi istochnik, pogruzhennyi v tipichnuyu pul'sarnuyu tumannost'), no teper' my uvereny v tom, chto eto imenno neitronnaya zvezda, prichem - molodaya. Avtory polagayut, chto mnogie neotozhdestvlennye gamma-istochniki v oblastyah zvezdoobrazovaniya - eto molodye pul'sary. I GLAST-Fermi smozhet ih vyyavit'.


Vypusk 196. 01-12 oktyabrya 2008

arxiv:0810.1512 O galakticheskom tempe rozhdeniya neitronnyh zvezd (On the birthrates of galactic neutron stars)
Authors: E.F. Keane, M. Kramer
Comments: accepted for publication in MNRAS, 9 pages, 3 figures

Sushestvuet neskol'ko populyacii otnositel'no molodyh odinochnyh neitronnyh zvezd: pul'sary, Velikolepnaya semerka, SGRs, AXPs, RRATs, CCOs ... Evolyucionnye svyazi mezhdu nimi neponyatny. Krome togo, skladyvaetsya paradoksal'naya situaciya: summa ocenok tempa rozhdeniya kazhdoi populyacii prevoshodit ocenku galakticheskogo tempa sverhnovyh. Znachit, vryad li mozhno oboitis' bez predpolozheniya o tom, chto kakie-to iz populyacii prinadlezhat odnomu evolyucionnom treku.

Avtory zashishayut ideyu o tom, chto pul'sary, RRATs i Velikolepnaya semerka - eto raznye proyavleniya odnogo evolyucionnogo treka (t.e., prosto my vidim raznye stadii evolyucii).

Lichno mne seichas kazhetsya, chto bolee veroyaten drugoi scenarii, zashishaemyi, naprimer, Hose Ponsom. A imenno. Raspad magnitnogo polya i nagrev kory pozvolyaet postroit' cepochku SGRs, AXPs -> Velikolepnaya semerka, RRATs i pul'sary s bol'shim magnitnym polem.


arxiv:0810.1527 Pul'sary kak istochniki kosmicheskih pozitronov vysokih energii (Pulsars as the sources of high energy cosmic ray positrons)
Authors: Dan Hooper et al.
Comments: 10 pages, 5 figures

Vsem pamyatna nedavnyaya diskussiya po rezul'tatam raboty sputnika PAMELA. Na neskol'kih konferenciyah komanda sputnika dolozhila ob obnaruzhenii izbytka pozitronov. T.e., standartnye modeli rozhdeniya etih chastic v mezhzvezdnoi srede ne mogut ob'yasnit' predstavlennye rezul'taty. Otsyuda mnogie sdelali vyvod, chto effekt mozhet naiti ob'yasnenie v rozhdenii elektron-pozitronnyh par pri annigalyacii chastic temnoi materii.

V etoi stat'e avtory obsuzhdayut kuda bolee konservativnuyu gipotezu o tom, chto izbytok pozitronov mozhet porozhdat'sya pul'sarami. Dlya ob'yasneniya vsego izbytka im trebuetsya dostatochno vysokii temp rozhdeniya gamma-pul'sarov vo vsei Galaktike, a takzhe dostatochnaya aktivnost' blizkih ob'ektov. Poka vse ukladyvaetsya v izvestnye ogranicheniya. Skoree vsego, okonchatel'nyi otvet dadut dannye sputnika GLAST-Fermi, kotorye poyavyatsya uzhe v blizhaishii god-dva.

Kstati, o planiruemyh nabldeniyah pul'sarov na GLAST-Fermi mozhno prochest' tut arxiv:0810.1637.


Vypusk 195. 12-30 sentyabrya 2008

obzor arxiv:0809.4228 Kvarkovoe veshestvo v kompaktnyh zvezdah: astrofizicheskie prilozheniya i vozmozhnye proyavleniya (Quark matter in compact stars: astrophysical implications and possible signatures)
Authors: I. Bombaci
Comments: 24 pages, Invited talk at "the Eleventh Marcel Grossman Meeting on General Relativity", Berlin 2006

Bol'shoi obzor po kvarkovym zvezdam i svyazannoi s etim fizikoi. Formul malo - t.e., napisano ponyatno. Privedeny osnovnye sovremennye kandidaty (hotya, pozhalui, seichas oni kazhutsya menee sil'nymi, chem neskol'ko let nazad). Dan horoshii istoricheskii obzor. Bolee 100 ssylok.


arxiv:0809.4231 Opticheskie i infrakrasnye vspyshki ot tranzientnogo gallakticheskogo istochnika povtoryayushihsya gamma-vspleskov (Optical and infrared flares from a transient Galactic soft gamma-ray repeater)
Authors: A.J. Castro-Tirado et al.
Comments: 20 pages, Version submitted to Nature on 31 Jan 2008. A substantially revised version of this work has been published in Nature, vol. 455 issue 7212 pp 506-509 under the title "Flares from a Galactic magnetar suggest a missing link to dim isolated neutron stars"

Srazu dve gruppy (sm. vtoruyu stat'yu arxiv:0809.4043) dokladyvayut ob obnaruzhenii interesnogo opticheskogo tranzienta.

Tranzient nablyudalsya posle gamma-vspleska. Vsplesk byl obnaruzhen 10 iyunya 2007 goda sputnikom SWIFT. Srazu stalo yasno, chto eto skoree vsego kakoi-to galakticheskii ob'ekt, a ne kosmologicheskii gamma-vsplesk. Eto sledovalo ne tol'ko iz togo, chto istochnik lezhit v ploskosti Galaktiki, no i iz ryada drugih svoistv.

Zatem, pribor RXT obnaruzhil rentgenovskuyu vspyshku. Takzhe bylo obnaruzheno i opticheskoe izluchenie. Sperva vsya summa dannyh ukazyvala na to, chto eto mozhet byt' dvoinaya sistema s chernoi dyroi (bystraya rentgenovskaya novaya).

Odnako novye dannye govoryat o drugom. V rassmatrivaemyh stat'yah avtory soobshayut o nablyudenii neskol'kih desyatkov opticheskih vspyshek, ochen' pohozhih na rentgenovskie vspyshki magnitarov. Vrode by est' ukazaniya na harakternyi period okolo 7 sekund. Poetomu obe gruppy interpretiruyut dannye, kak opticheskoe izluchenie magnitara. Togda eto budet pervoe takoe opticheskoe nablyudenie. Odnako ne isklyucheno, chto mogut poyavit'sya i drugie modeli.


Vypusk 193. 15-31 avgusta 2008

arxiv:0808.1899 Vspyhivayushii radiotranzient v napravlenii galakticheskogo centra (A bursting radio transient in the direction of the galactic center)
Authors: Paul S. Ray et al.
Comments: 11 pages, 2 figures, to appear in proceedings of "Bursts, pulses and flickering: wide-field monitoring of the dynamic radio sky"

GCRT J1745-3009 - interesnyi i neponyatnyi radiotranzient, otkrytyi neskol'ko let nazad. Obsuzhdalos' neskol'ko raznyh modelei istochnika, i mozhno pridumat' novye (naprimer, odinochnye neitronnye zvezdy na ekzoticheskih stadiyah, superezhektor v dvoinoi sisteme i tp.). Avtory opisyvayut dannye po etomu istochniku, obsuzhdayut nekotorye modeli i rassuzhdayut, chto mozhno nadeyat'sya uznat' v budushem.


arxiv:0808.2034 Rentgenovskie pul'sary glazami INTEGRAL (X-ray pulsars through the eyes of INTEGRAL)
Authors: A. Lutovinov, S. Tsygankov
Comments: 12 pages, 8 figures

Daetsya obzor rezul'tatov po nablyudeniyam rentgenovskih pul'sarov na sputnike INTEGRAL. Naibolee interesno opisanie zavisimosti energii ciklotronnoi linii ot svetimosti (eto izmereno dlya treh istochnikov). Takzhe rassmatrivaetsya evolyuciya periodov i zavisimost' doli pul'siruyushego ot razlichnyh parametrov.


arxiv:0808.2292 Mul'titeleskopnyi taiming PSR J1518+4904 (Multi-telescope timing of PSR J1518+4904)
Authors: G.H.Janssen et al.
Comments: 11 pages, 8 figures, accepted by A&A

PSR J1518+4904 - eto odna iz devyati sistem, sostoyashih iz dvuh neitronnyh zvezd (hotya by odna iz kotoryh yavlyaetsya radiopul'sarom). Avtory detal'no issleduyut istochnik i poluchayut ochen' interesnyi rezul'tat.

Vo-pervyh, udalos' tochno izmerit' polnuyu massu sistemy - 2.72 massy Solnca. Tut poka nichego udivitel'nogo. Interesno, chto odna iz neitronnyh zvezd (ta, kotoraya yavlyaetsya pul'sarom) imeet nizkuyu massu: 0.72+0.51/-0.58 mass Solnca. Predely sootvetstvuyut veroyatnosti 95.4 procenta. V principe, verhnii predel v 1.17 solnechnyh mass ne kazhetsya takim uzh udivitel'nym, no vspomnite, chto my govorim o millisekundnom pul'sare, kotoryi byl raskruchen za schet akkrecii so vtorogo kompan'ona! T.e., vo-pervyh, nachal'naya massa byla eshe men'she, a vo-vtoryh, kompan'on, kotoryi dolzhen byl obrazovat'sya iz iznachal'no menee massivnoi zvezdy, zametno tyazhelee pul'sara (massa kompan'ona 1.55-2.58 solnechnyh mass s toi zhe dostovernost'yu 95.4 procenta).

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


Vypusk 192. 01-14 avgusta 2008

miniobzor arxiv:0808.1279 Ogranicheniya na uravnenie sostoyaniya yadernoi materii pri vysokoi plotnosti po nablyudeniyam neitronnyh zvezd (Constraints on the High-Density Nuclear Equation of State from Neutron Star Observables)
Authors: David Blaschke, Thomas Klaehn, Fridolin Weber
Comments: 16 pages, 11 figures, Contribution to Proceedings of the 3rd International Workshop on Astronomy and Relativistic Astrophysics (IWARA), 3-6 October 2007, Joao Pessoa, Brazil

Ocherednoi obzor po astrofizicheskim ogranicheniyam na uravnenie sostoyaniya pri vysokoi plotnosti. Bystrovrashayushiesya i massivnye neitronnye zvezdy, kompaktnye ob'ekty s izmerennym radiusom, ochen' goryachie ili holodnye ... vse oni mogut dat' informaciyu o tom, kak vedet sebya veshestvo v ih nedrah pri plotnosti, v neskol'ko raz prevoshodyashei yadernuyu.


arxiv:0808.1594 Ochen' vysokotochnaya VLBI-astrometriya dlya pul'sara PSR J0437-4715 i prilozheniya k teoriyam gravitacii (Extremely high precision VLBI astrometry of PSR J0437-4715 and implications for theories of gravity)
Authors: A. T. Deller, J.P.W. Verbiest, S.J. Tingay, M. Bailes
Comments: 11 pages, 1 Figure, submitted to ApJL

Avtory rasskazyvayut o tochnom opredelenii (tochnost' okolo 1%) parallaksa do samogo blizkogo (156 pk) millisekundnogo dvoinogo pul'sara i o tom, chto iz etogo mozhno izvlech'. A izvlech' mozhno nemalo, t.k. dlya takih ob'ektov est' nezavisimye metody opredeleniya rasstoyaniya. Eti nezavisimye metody osnovany na nekotoryh predpolozheniyah, kotorye mozhno proveryat', ispol'zuya tochnyi trigonometricheskii parallaks. Sredi etih prepolozhenii vo-pervyh nado otmetit' postoyanstvo postoyannoi tyagoteniya (n'yutonovoi). I avtory privodyat samyi zhestkii predel na ee proizvodnuyu. Vo-vtoryh, eto neizvestnye massivnye planety na zadvorkah solnechnoi sistemy. I v tret'ih, gravitacionno-volnovoi shum.

Podrobnee ob izmerenii parallaksov pul'sarov s pomosh'yu VLBI sm. arxiv:0808.1598. V chastnosti, tam rasskazyvaetsya ob izmereniyah s submilliarksekundnoi tochnost'yu (tochno opredeleno rasstoyanie do pul'sara na ~2.5 kpc ot nas).


Vypusk 191. 22-31 iyulya 2008

arxiv:0807.5013 Vysokotochnaya geometriya dvuhpolyusnogo pul'sara (High-precision geometry of a double-pole pulsar)
Authors: M. Kramer, S. Johnston
Comments: accepted for publication in MNRAS, 7 pages, 4 figures

Avtory detal'no issleduyut interesnyi radiopul'sar, kotoryi, vozmozhno, stanet odnim iz rozettskih kamnei (odnim vryad li oboidutsya) dlya ponimaniya raboty pul'sarnogo mehanizma.

Pul'sar B0906-49 demonstriruet dva impul'sa za period. Avtory nadezhno pokazyvayut, chto eto imenno impul'sy ot raznyh polyusov i tshatel'no issleduyut geometriyu ob'ekta. Dostoverno pokazano, chto istochnik yavlyaetsya ortogonal'nym rotatorom, t.e. ego magnitnaya os' perpendikulyarna osi vrasheniya. Opredelena vysota, na kotoroi voznikaet izluchenie (okolo 230 km). Avtory polagayut, chto istonik mozhet byt' zaregistrirovan GLAST v gamma-diapazone. Togda, v samom dele, eto budet otlichni probnyi kamen' dlya razrabotchikov teorii izlucheniya pul'sarov.


Vypusk 190. 09-21 iyulya 2008

arxiv:0807.2088 Poisk na vysokih chastotah radiopul'sarov v boksah EGRET (A high frequency search for radio pulsars in EGRET error boxes)
Authors: M.J. Keith et al.
Comments: 5 pages, accepted for publication in MNRAS

Izvestno, chto v kataloge gamma-detektora EGRET okolo poloviny istochnikov ne otozhdestvleny. Predpolagaetsya, chto mnogie iz nih mogut byt' radiopul'sarami. Okolo goda nazad gruppa avtorov provodila glubokii poisk pul'sarov v 56 boksah oshibok, nichego ne bylo obnaruzheno. V etoi stat'e govorit'sya o poiske v treh oblastyah lokalizacii. No tut rech' idet uzhe o bolee vysokih chatostah - 3.1 GGc.

Obnaruzhen pul'sar PSR J1028-5819 s periodom okolo 90 millisekund. Avtory polagayut, chto on i yavlyaetsya odnim iz treh gamma-istochnikov. Na nizkih chastotah tam nichego ne bylo naideno, tak chto, vozmozhno, i dlya drugih oblastei poisk stoit povtorit' na vysokih chastotah.


arxiv:0807.2106 Proishozhdenie i evolyuciya magnitarov (Origin and evolution of magnetars)
Authors: Lilia Ferrario, D.T. Wickramasinghe
Comments: 5 pages, 2 figures, accepted for publication in the MNRAS (letters)

Avtory, yavlyayushiesya storonnikami togo, chto magnitnye polya magnitarov dostalis' im v nasledstvo ot zvezd-praroditelei, a ne byli sgenerirovany na stadii protoneitronnoi zvezdy, provodyat populyacionnyi sintez magnitarov. Razumeetsya, dlya populyacionnoi modeli avtoram prihoditsya delat' ryad predpolozhenii, mnogie iz kotoryh mozhno osparivat'. Tem ne menee, popytka dovol'no interesnaya.


arxiv:0807.2644 Relyativistskaya precessiya v sisteme dvoinogo pul'sara (Relativistic spin precession in the double pulsar)
Authors: Rene P. Breton et al.
Comments: 28 pages, 6 figures, 1 table, 2 movies; Science, 04 July 2008, Vol. 321, no. 5885, pp. 104-107

Osnovyvayas' na ne samyh pryamyh dannyh, avtory vytaskivayut iz nablyudenii precessiyu sobstvennogo momenta neitronnoi zvezdy (pul'sara B) otnositel'no polnogo orbital'nogo momenta sistemy. Eto pozvolyaet proverit' predskazanie OTO, kotoroe vypolneno s tochnost'yu okolo 13 procentov. Razumeetsya, s dal'neishimi nablyudeniyami tochnost' budet vozrastat'.


Vypusk 186. 16-31 maya 2008

arxiv:0805.2396 Millisekundnyi dvoinoi pul'sar s ekscentrichnoi orbitoi v ploskosti Galaktiki (An Eccentric Binary Millisecond Pulsar in the Galactic Plane)
Authors: D. J. Champion et al.
Comments: 28 pages, 4 figures inc Supplementary On-Line Material. Accepted for publication in Science, published on Science Express: 10.1126/science.1157580

Obnaruzhen interesnyi dvoinoi millisekundnyi pul'sar. Po otdel'nosti ego svoistva ne byli by stol' interesny, no ih kombinaciya zadaet zagadki. Eto millisekundnyi (2.15 msek) pul'sar, u kotorogo kompan'onom yavlyaetsya normal'naya zvezda solnechnoi massy, pri etom orbita imeet vysokii ekscentrisitet (0.44) i bol'shoi period (95 dnei), a nahoditsya sistema v ploskosti Galaktiki. Krome togo, ocenka massy neitronnoi zvezdy daet 1.7-1.8 mass Solnca (no eta velichina eshe mozhet, na moi vzglyad, preterpet' pereocenku).

Zagadka v tom, chto standartnye evolyucionnye shemy ne dayut takih sistem. Est' neskol'ko variantov ekzotichnosti, obsuzhdaemyh avtorami. Pervyi: pul'sar takim i rodilsya. Vtoroi: eto byla troinaya sistema. Tretii: pul'sar popal v ploskost' Galaktiki iz sharovogo skopleniya. Scenarii s troinoi vyglyadit naibolee privlekatel'nym.


arxiv:0805.2586 Vozmozhnoe opticheskoe otozhdestvlenie starogo blizkogo pul'sara J0108-1431 (A possible optical counterpart to the old nearby pulsar J0108-1431)
Authors: R.P. Mignani, G.G. Pavlov, O. Kargaltsev
Comments: 5 pages, 4 figures, submitted to A&A

Avtory raportuyut o vozmozhnom obnaruzhenii v opticheskom diapazone blizkogo (130 pk) starogo (166 millionov let) radiopul'sara. Vse govorit o teplovom izluchenii (T=90 000K) vsei poverhnosti (R=13 km) neitronnoi zvezdy. Esli eto i v samom dele tak, to eto ves'ma interesno, t.k. standartnye modeli ohlazhdeniya (bez dopolnitel'nyh istochnikov tepla, naprimer iz-za raspada magnitnyh polei ili vnutrennego treniya) ne dayut takie temperatury dlya stol' staryh ob'ektov.


arxiv:0805.4758 Pobit predel na gravitacionnye volnya ot pul'sara v Krabe po dannym i zamedlenii (Beating the spin-down limit on gravitational wave emission from the Crab pulsar)
Authors: The LIGO Scientific Collaboration: B. Abbott, et al
Comments: 6 pages, 1 figure

Po rezul'tatam neskol'kih mesyacev nablyudenii komanda LIGO smogla postavit' pryamoi (t.e. poluchennyi po dannym gravvolnovogo detektora) predel na gravizluchenie ot pul'sara v Krabe. I predel etot luchshe kosvennogo predela, poluchennogo po detal'nomu taimingu pul'sara.

S odnoi storony, rezul'tat nulevoi. S drugoi - LIGO eshe raz pokazyvaet, chto predely, ustanavlivaemye etim eksperimentom, luchshe kosvennyh.


Vypusk 184. 21-30 aprelya 2008

arxiv:0804.3838 Mnogochastotnye integrirovannye profili pul'sarov (Multi-frequency integrated profiles of pulsars)
Authors: Simon Johnston, Aris Karastergiou, Dipanjan Mitra, Yashwant Gupta
Comments: Accepted for publication in MNRAS. 15 pages

Avtory predstavlyayut nablyudeniya 67 pul'sarov na chastotah ot 243 MGc (na teleskope GMRT v Indii) do 3.1 GGc (na teleskope Parkes v Avstralii). V stat'e privodyatsya profili dlya 34 pul'sarov s bol'shim otnosheniem signal/shum. Avtory obsuzhdayut svoistva pul'sarov s raznymi vozrastami. V chastnosti, oni polagayut, chto oblast' v magnitosfere, v kotoroi proishodit izluchenie, evolyucioniruet po mere zamedleniya tempa vrasheniya pul'sara (chem starshe, tem nizhe v magnitosfere voznikaet izluchenie).


arxiv:0804.4318 Populyaciya pul'sarov s interpul'sami i prilozheniya k evolyucii diagrammy napravlennosti (The population of pulsars with interpulses and the implications for beam evolution)
Authors: Patrick Weltevrede, Simon Johnston
Comments: 7 pages, 2 figures, accepted for publication in MNRAS

Avtory rassmatrivayut vopros ob izmenenii ugla mezhdu magnitnoi os'yu i os'yu vrasheniya u pul'sarov s tochki zreniya doli istochnikov s interimpul'som. Interimpul's voznikaet, esli ugol mezhdu osyami blizok k 90 gradusam, togda my vidim signal ot dvuh polyarnyh shapok (eshe vozmozhna situaciya, kogda osi naoborot pochti sonapravleny, a puchok pul'sarnogo izlucheniya ochen' shirok, no, davaite, vmeste s avtorami stat'i, konservativno isklyuchim takuyu vozmozhnost'). Ocenki pokazyvayut, chto okolo 5 procentov pul'sarov dolzhny davat' interimpul'sy, esli lyubye ugly mezhdu osyami ravnoveroyatny. Odnako nablyudeniya pokazyvayut, chto dolya men'she (okolo 1.8 procenta). Prichem, dlya pul'sarov s dlinnymi periodami dolya men'she, chem dlya pul'sarov s korotkimi. Avtory rassmatrivayut raznye neslozhnye modeli, kotorye mogli by eto ob'yasnit'. Po mneniyu avtorov naibolee razumnaya model' dolzhna vklyuchat' postepennoe shozhdenie osei. Esli process idet eksponencial'no, to harakternoe vremya poluchaetsya okolo 108 - 109 let.

Konechno, zhizn' mozhet byt' ustroena slozhnee, chem prostye modeli.


Vypusk 183. 01-20 aprelya 2008

arxiv:0804.0832 Rassheplenie fotonov i rozhdenie par v sil'nyh magnitnyh polyah (Photon Splitting and Pair Conversion in Strong Magnetic Fields)
Authors: Matthew G. Baring
Comments: 18 pages, 3 embedded figures, invited review, to appear in Proc. CASYS '07 Conference "Computing Anticipatory Systems," eds. D. Dubois, et al. (AIP Conf. Proc., New York, 2008)

V sil'nyh magnitnyh polyah fotony mogut v odinochku rozhdat' elektron-pozitronnye pary, a takzhe prevrashat'sya v dva fotona men'shei energii. V stat'e rassmatrivayutsya oba processa, a takzhe opisyvaetsya, chto v svyazi s etim mozhet uvidet' zapuskaemyi cherez mesyac sputnik GLAST.

Posle kratkogo vvedeniya, pervuyu chast' avtor posvyashaet teorii, a vtoruyu - prilozheniyam k astronomii. Mozhno uznat' massu interesnogo. Naprimer, esli chast' kosmicheskih luchei sverhvysokih energii yavlyaetsya fotonami (chto, pravda, malo veroyatno), to, vzaimodeistvuya s zemnym magnitnym polem, oni mogut davat' elektron-pozitronnye pary. I sledy takih processov ishut na sootvetstvuyushih ustanovkah.


Vypusk 182. 18-31 marta 2008

arxiv:0803.2691 Otkrytie dvuh magnitnyh massivnyh zvezd v skoplenii Tumannosti Oriona: klyuch k proishozhdeniyu magnitnyh polei neitronnyh zvezd? (Discovery of two magnetic massive stars in the Orion Nebula Cluster: a clue to the origin of neutron star magnetic fields?)
Authors: V. Petit, G.A. Wade, L. Drissen, T. Montmerle, E. Alecian
Comments: 6 pages, Accepted by MNRAS

Kak izvestno, proishozhdenie magnitnyh polei neitronnyh zvezd, osobenno magnitarov, ostaetsya tainoi. To li pole generiruetsya na stadii protoneitronnoi zvezdy, to li yadro zvezdy-praroditelya imelo sil'noe pole, kotoroe posle kollapsa yadra stalo polem neitronnoi zvezdy. U obeih gipotez est' svoi problemy. Odnoi iz problem gipotezy o reliktovom pole yavlyaetsya maloe kolichestvo izvestnyh magnitnyh massivnyh zvezd.

V stat'e avtory raportuyut ob otkrytii dvuh massivnyh zvezd s polyami poryadka kilogaussa.

Na moi vzglyad, mozhet vozniknut' odna problema. Delo v tom, chto vse izvestnye magnitary - odinochnye. Hotya nikakoi selekcii v pol'zu etogo net. Mezhdu tem, iz treh magnitnyh massivnyh zvezd dve vhodyat v kratnye sistemy. Konechno, daleko ne vse dvoinye perezhivut vzruv sverhnovoi. Tem ne menee, imeya uzhe bolee 10 kandidatov v magnitary, stoit zadumat'sya nad ih odinochnost'yu.


arxiv:0803.3818 Teoreticheskaya model' dlya gigantskoi vspyshki magnitara po obrazu solnechnoi vspyshki (Solar-type Theoretical Model for Magnetar Giant Flare)
Authors: Youhei Masada, Shigehiro Nagataki, Kazunari Shibata, Toshio Terasawa
Comments: submitted to ApJ, 6 pages, 3 figures

Avtory stroyat prostuyu model' dlya gigantskih magnitarnyh vspyshek (tipa 27 dekabrya 2004 goda), osnovyvayas' na modeli solnechnoi vspyshki. Osnovnym dostoinstvom, na moi vzglyad, yavlyayutsya naglyadnost' modeli i vozmozhnost' delat' prostye ocenki s ee ispol'zovaniem.


Vypusk 181. 01-17 marta 2008 goda

arxiv:0803.1373 1E161348-5055 v ostatke sverhnovoi RCW 103: magnitar v malomassivnoi dvoinoi sisteme? (1E161348-5055 in the Supernova Remnant RCW 103: A Magnetar in a Young Low Mass Binary System?)
Authors: Fabio Pizzolato et al.
Comments: 33 pages, Accepted for publication in the ApJ

Avtory v detalyah razvivayut model', soglasno kotoroi semichasovoi period i central'nogo kompaktnogo istochnika 1E161348-5055 v ostatke sverhnovoi RCW 103 ob'yasnyaetsya kak orbital'nyi period malomassivnoi dvoinoi sistemy. V takoi modeli sistema pohozha na izvestnye sistemy s belymi karlikami - polyary. Kompaktnyi ob'ekt imeet ochen' bol'shoe magnitnoe pole, i vtoroi komponent okazyvaetsya vnutri magnitosfery. V rezul'tate veshestvo s normal'noi zvezdy mozhet legko peretekat' na kompaktnyi ob'ekt.


arxiv:0803.2104 Ocenka nachal'nogo perioda pul'sarov po nablyudeniyam pul'sarnyh tumannostei na GLAST/LAT (Estimating the birth period of pulsars through GLAST/LAT observations of their wind nebulae)
Authors: O.C. de Jager
Comments: 10 pages, no figures. To appear in Astrophysical Journal Letters

Avtor pokazyvaet, chto pri izvestnom sovremennom periode i razumnyh predpolozheniyah gamma-potok ot pul'sarnyh tumannostei zavisit v osnovnom ot nachal'nogo perioda nakachivayushego tumannost' pul'sara. Zapuskaemyi v etom godu sputnik GLAST smozhet, takim obrazom, hotya by kachestvenno ocenit' nachal'nye periody dlya populyacii radiopul'sarov.



Vypusk 180. 14-29 fevralya 2008 goda

arxiv:0802.1923 Rezonansnoe ciklotronnoe rasseyanie v izluchenii magnitarov (Resonant cyclotron scattering in magnetars' emission)
Authors: Nanda Rea, Silvia Zane, Roberto Turolla, Maxim Lyutikov, Diego Gotz
Comments: 42 pages, 11 figures. ApJ submitted on 2007 December 11

Avtory ispol'zuyut model', v kotoroi neteplovoi spektr magnitarov na energiyah poryadka neskol'kih keV ob'yasnyaetsya rezonansnym rasseyaniem fotonov teplovogo izlucheniya poverhnosti na goryachei magnitosfernoi plazme. Oni sravnivayut model'nye rezul'taty s dannymi po mnogim ARP i MPG (AXP, SGR). Rezul'taty govoryat o tom, chto plotnost' elektronov v magnitosfere na tri poryadka vyshe Goldraih-Dzhulianovskoi plotnosti.


miniobzor arxiv:0802.2227 Neitronnye zvezdy i ih magnitnye polya (Neutron stars and their magnetic fields)
Authors: Andreas Reisenegger
Comments: To appear in Revista Mexicana de Astronomia y Astrofisica, as part of the proceedings of the XII Latin American Regional IAU Meeting, held on Isla Margarita, Venezuela, 22-26 October 2007. Spanish and English abstract, English text, 7 pages, no figures

Nebol'shoi tolkovyi obzor po neitronnym zvezdam. Avtor - specialist po magnitnym polyam etih ob'ektov. No, prezhde chem pereiti sobstvenno k polyam, on kratko, no ochen' chetko obrisovyvaet osnovnuyu fiziku, svyazannuyu s neitronnymi zvezdami. Bukval'no desyatok prostyh formul, umestivshihsya vmeste s ob'yasneniyami na pare stranic, dayut yasnuyu kartinku.


arxiv:0802.2571 Elektrodinamika magnitarov III. (Electrodynamics of Magnetars III: Pair Creation Processes in an Ultrastrong Magnetic Field and Particle Heating in a Dynamic Magnetosphere)
Authors: Christopher Thompson
Comments: 25 pages, submitted to the Astrophysical Journal

Stat'i Krisa Tompsona - odnogo izv edushih specialistom po elektrodinamike magnitarov- chasto pechatayut v odnu kolonku, a ne v dve, t.k. inache formuly ne umeshayutsya. Ocherednaya stat'ya - ne isklyuchenie.

Stat'ya v osnovnom posvyashena detal'nomu izucheniyu processa rozhdeniya par v sil'nyh magnitnyh polyah.

Sm. takzhe eshe odnu stat'yu Tompsona po magnitaram arxiv:0802.2572, a takzhe rabotu arxiv:0802.2647, posvyashennuyu modelirovaniyu spektrov magnitarov.


arxiv:0802.2963 Rentgenovskie nablyudeniya parsekovyh hvostov za dvumya pul'sarami srednego vozrasta (X-ray Observations of Parsec-Scale Tails behind Two Middle-Aged Pulsars)
Authors: O. Kargaltsev, Z. Misanovic, G. G. Pavlov, J. A. Wong, G. P. Garmire
Comments: 14 pages, 16 figures and 5 tables

Nablyudeniya na Chandre i N'yutone pokazali nalichie simpatichnyh hvostikov (kazhdyi dlinoi v neskol'ko parsek), tyanushihsya za dvumya radiopul'sarami.


Hvost pul'sara PSR J1509-5850. Krasnym pokazano rentgenovskoe izobrazhenie, a sinim - radio.

Takie hvosty ne redkost', poskol'ku pul'sary dvizhutsya v srede so sverhzvukovoi skorost'yu, i sootnoshenie davlenii takovo, chto obrazuetsya udarnaya volna. Hvosty pomogayut tochno opredelit' napravlenie dvizheniya pul'sara. Inogda eto vazhno. Naprimer dlya PSR J1740+1000 okazalos', chto on rodilsya vysoko nad ploskost'yu galaktiki i seichas dvizhetsya v ee storonu, t.e. praroditelem byla ne zvezda diska Galaktiki (kak eto chashe vsego byvaet), a zvezda galo. Tak chto "po hvostu mozhno opredelit' rodoslovnuyu".


Vypusk 179. 01-14 fevralya 2008 goda

miniobzor arxiv:0802.0391 Izuchenie akkreciruyushih neitronnyh zvezd i chernyh dyr s pomosh'yu vremennyh ryadov: za stepennym spektrom (Studying accreting black holes and neutron stars with time series: beyond the power spectrum)
Authors: S. Vaughan, P. Uttley
Comments: 13 pages, 6 figures, in "Noise and Fluctuations" Proc. SPIE vol. 6603

Akkreciya na neitronnye zvezdy i chernye dyry idet ne rovnym spokoinym potokom. Est' turbulentnye dvizheniya, razlichnye neustoichivosti i tp. Vse eto otrazhaetsya na krivoi bleska istochnika, na taiminge i td. Razumeetsya, astronomy "oborachivayut" zadachu: po taimingu, po nablyudeniyam fluktuacii svetimosti i drugim menyayushimsya harakteristikam oni pytayutsya uznat' chto-to novoe o processe akkrecii. O nekotoryh novostyah v takih issledovaniyah mozhno uznat' ih obzora.

Sm. takzhe stat'yu arxiv:0802.0376, posvyashennuyu analogichnomu voprosu, no tol'ko isklyuchitel'no dlya sistem s chernymi dyrami.


arxiv:0802.0494 Magnitar 1E 1547.0-5408: radiospektr, polyarimetriya i taiming (The magnetar 1E 1547.0-5408: radio spectrum, polarimetry, and timing)
Authors: F. Camilo et al.
Comments: Accepted for publication in ApJ (7 pages, including 6 figures)

Avtory pronablyudali radioizluchenie ot odnogo iz anomal'nyh rentgenovskih pul'sarov. Voobshe, stacionarnoe radioizluchenie dlya magnitarov netipichno. Sobstvenno, ono izvestno eshe tol'ko ot odnogo ob'ekta - AXP J1810-197, da i to tam ono vozniklo posle vspyshki. U 1E 1547.0-5408 radioizluchenie stabil'no. Sam istochnik nahoditsya v ostatke sverhnovoi i obladaet dovol'no udivitel'nymi svoistvami.

Naprimer, radiospektr prakticheski ploskii ot 1 do 40 GGc. Proizvodnaya perioda u nego rastet (t.e. istochnik zamedlyaetsya vse bystree), hotya rentgenovskaya svetimost' pri etom umen'shalas'. Teper' ona dazhe nachala rasti, no kakih-to yavnyh izmenenii v tempe evolyucii proizvodnoi perioda ne sluchilos'. V obshem, interesnyh dannyh navalom, a kartina yasnee ne stanovitsya.


arxiv:0802.0815 Peresmotr v storonu umen'sheniya rasstoyaniya do skopleniya 1806-20 i svyazannogo s nim magnitara po spektroskopicheskim dannym v blizhnem IK-diapazone, poluchennym na teleskopah Gemini (A downward revision to the distance of the 1806-20 cluster and associated magnetar from Gemini near-Infrared spectroscopy)
Authors: J. L. Bibby et al.
Comments: 6 pages, 4 figures, accepted for MNRAS Letters

Vse pomnyat gipervspyshku odnogo iz istochnikov myagkih povtoryayushihsya gamma-vspleskov (MPG), nablyudavshuyusya 27 dekabrya 2004 goda. Razumeetsya, tochnaya ocenka energetiki vspyshki trebuet tochnogo znaniya rasstoyaniya do istochnika. Ono neizvestno. Tradicionno ispol'zuetsya znachenie 15 kpk. V takom sluchae istochnik nahoditsya za centrom Galaktiki primerno na takom zhe udalenii, kak i Solnce. Takaya vysokaya ocenka rasstoyaniya poluchena po dannym CO nablyudenii, a takzhe po dannym o kinematicheskih svoistvah odnoi iz yarkih (LBV) zvezd v skoplenii, v kotorom, kak polagayut, nahoditsya magnitar. Est' i drugie ocenki, kotorye pridvigayut MPG blizhe k nam.

V stat'e avtory snova pytayutsya ocenit' rasstoyanie do zvezdnogo skopleniya, ispol'zuya spektroskopicheskie dannye. T.e., ideya sostoit v tom, chtoby po spektram tochno opredelit' spektral'nye klassy zvezd. Nu a zatem mozhno budet sdelat' ocenku rasstoyaniya do nih. Avtory poluchayut velichinu 7-10 kpk. Esli eta ocenka verna, to energetika vspyshki stanovitsya men'she v 3-4 raza. Pochemu eto tak vazhno? Potomu chto, osnovyvayas' na ocenke energetiki etoi vspyshki mnogie avtory pytalis' ocenit' nablyudaemost' takih vspyshek v blizkih galaktikah. Esli svetimost' vspleska byla v 4 raza men'she, chem obsheprinyataya ocenka, to sil'no smyagchaetsya paradoks otsutstviya mnogchislennyh analogichnyh yavlenii ot vnegalakticheskih MPG v dannyh gamma-detektorov (naprimer, BATSE).


arxiv:0802.0881 Glubokii analiz nullinga pul'sarov na teleskope v Aresibo otkryvaet eshe bol'she sluchaev pereiodicheskogo povedeniya (Deep Analyses of Nulling in Arecibo Pulsars Reveal Further Periodic Behavior)
Authors: Jeffrey Herfindal, Joanna Rankin
Comments: 5 pages, 2 figures, 2 tables, uses mn2e.cls

Nulling - eto propadanie impul'sa pul'sara. Takoe yavlenie nablyudaetsya u mnogih ob'ektov: prishlo vremya uvidet' pul's, a nichego net, nul'. Propushennye impul'sy vstrechayutsya primerno u poloviny pul'sarov i u nekotoryh sostavlyayut do 70 procentov impul'sov. U kakih-to pul'sarov impul'sy propuskayutsya po odinochke, kakie-to mogut zamolkat' na chasy. Pochemu tak proishodit neyasno, chto ne udivitel'no, poskol'ku net sobstvenno teorii pul'sarnogo izlucheniya (tochnee, est' neskol'ko konkuriruyushih modelei, vse iz kotoryh imeyut svoi problemy). Tem vremenem, nablyudeniya podkidyvayut novye zagadki. Okazyvaetsya, chto u nekotoryh pul'sarov v poyavlenie nullinga est' nekotoraya regulyarnost'.

Tak naprimer nedavno poyavilas' stat'ya arxiv:0802.0247, v kotoroi opisyvalos' kvaziperiodicheskoe poyavlenie "nulei" u pul'sara PSR J1819+1305. Ranee periodicheskii nulling byl otkryt u PSR B1133+16. V novoi stat'e privedeny dannye po eshe neskol'kim ob'ektam.

Vse nablyudeniya, opisannye v stat'e, provodilis' v Aresibo na 327 MGc. Pokazano, chto eshe neskol'ko pul'sarov pokazyvayut "kvaziperiodicheskih nulling", prichem harakternyi period poryadka 40-80 periodov obrasheniya.


arxiv:0802.1242 Peremennost' pul'sara PSR J1846-0258 s bol'shim magnitnym polem po dannym observatorii Chandra (Variability of the High-Magnetic Field X-ray Pulsar PSR J1846-0258 Associated with the Supernova Remnant Kes 75 as Revealed by the Chandra X-ray Observatory)
Authors: Harsha Sanjeev Kumar, Samar Safi-Harb
Comments: 5 pages, 3 figures, 1 table. Submitted to the Astrophysical Journal (Letters)

Interesnaya stat'ya s dostatochno epicheskim nazvaniem. Sut' vot v chem. PSR J1846-0258 - obladaet odnim iz samyh sil'nyh dlya radiopul'sarov magnitnym polem (pole, konechno, opredelyaetsya prosto po tempu zamedleniya pul'sara). On nahoditsya v ostatke sverhnovoi Kes 75. Avtory predstavili rentgenovskie dannye za 6 let. Za eto vremya potok rentgenovskogo izlucheniya vyros v 6 raz. Rost byl ne monotonnym, skoree mozhno govorit' o periode aktivnosti v 2006 g (sm. nizhe). Dlya radiopul'sarov eto sovershenno netipichno. Zato tipichno dlya magnitarov. T.o., razmyvaetsya eshe odna granica, razdelyayushaya podklasyy neitronnyh zvezd. Seichas uzhe vsem yasno, chto AXP i SGR - bliznecy-brat'ya. Nekotorye RRATs ochen' pohozhi na nekotorye radiopul'sary, a drugie (po drugim, ne radio, a rentgenovskim svoistvam) pohozhi na Velikolepnuyu semerku. Odin iz tranzientnyh AXP do nachala perioda aktivnosti klassificirovalsya kak central'nyi kompaktnyi istochnik v ostatke sverhnovoi (CCO). Hotya pri etom est' i bezuslovno otdel'nye tipy neitronnyh zvezd, tochno ne takie kak drugie (naprimer, slabozamagnichennye CCO c dostatochno dlinnym - sotni millisekund - nachal'nym periodom). Tak chto kartina astrofizicheskih proyavlenii neitronnyh zvezd stanovitsya vse slozhnee i pri etom postoyanno vidoizmenyaetsya.

Tut zhe poyavilas' i vtoraya stat'ya na etu temu. Prichem ona napisana dlya Science. Eti avtory uzhe raportuyut o nablyudeniyah magnitaro-podobnyh vspyshek ot pul'sara v Kes 75. Krome togo, oni privodyat bolee detal'nye dannye o periode aktivnosti v 2006 godu.


miniobzor arxiv:0802.1309 Registraciya gravitacionnyh voln, ispol'zuya vysokotochnye nablyudeniya pul'sarov (Gravitational wave detection using high precision pulsar observations)
Authors: G. Hobbs
Comments: 9 pages + figure, Accepted for publication in the JPCS issue for the Amaldi 7 proceedings

U pul'sarshikov svoi "nanodostizheniya": seichas vozmozhen taiming s tochnost' poryadka 100 nanosekund (konechno, rech' idet tol'ko o dostatochno stabil'nyh pul'sarah, kotoryh ne kolbasit pochem zrya). Takie dannye mozhno ispol'zovat' dlya samyh raznyh prilozhenii prosto potomu, chto takoi pul'sar ispol'zuetsya kak vysokotochnye chasy, kotorye podvergayutsya kakim-to vneshnim vozdeistviyam ili yavlyayutsya standartom, a vozdeistviyam podvergaetsya nablyudatel' na Zemle. Odnim iz takih vozdeistvii yavlyayutsya gravitacionnye volny.

V stat'e rasskazyvaetsya o tom, kak pul'sarnyi taiming mozhno ispol'zovat' dlya "nablyudeniya" gravitacionnyh voln. Kachestvenno ideya prosta (pervye vychisleniya prodelal 30 let nazad M. Sazhin v GAISh). Prohozhdenie gravitacionnoi volny cherez nablyudatel'nuyu sistemu na Zemle vyzyvaet "sboi" v nablyudaemom periode pul'sara. Nablyudaem neskol'ko pul'sarov. Sboi v nih, esli oni svyazany s samimi pul'sarami budut neskorellirovany. A vot esli sboi proishodit iz-za "potryaseniya" detektora, to u vseh pul'sarov v taiminge budet prisutstvovat' odna i tazhe osobennost'. Razumeetsya, tak mozhno zametit' gravitacionnye volny tol'ko s dostatochno bol'shim periodom (s nizkoi chastotoi). Takie volny nedostupny imeyushimsya detektoram (LIGO, VIRGO i dr.). Tak chto dve tehniki ne konkuriruyut, a dopolnyayut drug druga. Stol' nizkochastotnye gravitacionnye volny mogut byt' svyazany, naprimer, s parami sverhmassivnyh chernyh dyr v yadrah slivshihsya galaktik.


Vypusk 178. 22-31 yanvarya 2008 goda

arxiv:0801.4567 Igolka v stoge sena - Gde iskat' odinochnye ostyvayushie neitronnye zvezdy (The needle in the haystack - Where to look for more isolated cooling neutron stars)
Authors: The needle in the haystack - Where to look for more isolated cooling neutron stars Authors: B. Posselt, S.B. Popov, F. Haberl, J. Truemper, R. Turolla, R. Neuhaeuser
Comments: 14 pages, 9 figures, accepted by A&A

Ya redko pishu o svoih rabotah. Sobstvenno, eto vsego pyatyi sluchai za shest' let. No tut uderzhat'sya ne mogu: slishkom uzh dolgo my dobiralis' do prinyatiya stat'i v pechat'.

Vo-pervyh, v rabote predstavlena novaya versiya programmy populyacionnogo sinteza dlya rascheta evolyucii blizkih ostyvayushih neitronnyh zvezd. Vo-vtoryh, rezul'taty raboty ispol'zuyutsya dlya otveta na vopros o tom, gde iskat' novyh kandidatov. Ved' seichas Velikolepnaya semerka na kone. No esli za pervye pyat' let issledovaniya etih ob'ektov udalos' otkryt' semerku, to za sleduyushie pyat' - ni odnogo. V-tret'ih, v final'noi chasti stat'i obsuzhdayutsya "netradicionnye" idei po poisku novyh blizkih ostyvayushih neitronnyh zvezd.


Vypusk 177. 10-21 yanvarya 2008 goda

arxiv:0801.2589 Vysokotochnyi taiming PSR J0437-4715: dostovernoe rasstoyanie do pul'sara, vysokaya massa i predel na variaciyu n'yutonovskoi konstanty (Precision timing of PSR J0437-4715: an accurate pulsar distance, a high pulsar mass and a limit on the variation of Newton's gravitational constant)
Authors: J.P.W. Verbiest et al.
Comments: 19 pages, 4 figures, accepted for publication in The Astrophysical Journal

Pul'sar PSR J0437-4715 - blizhaishii millisekundnyi pul'sar. Ego nablyudayut s 1993 goda. Kompan'onom neitronnoi zvezdy yavlyaetsya belyi karlik. Sistema horosho izuchena, i v dannoi stat'e avtory predstavlyayut svezhie rezul'taty po opredeleniyu mnogih parametrov. S tochki zreniya fiziki, pozhalui, naibolee interesna ocenka massy neitronnoi zvezdy: 1.76+/-0.2 solnechnyh. Tut sushestvenno to, chto dlya deistvitel'no horosho izuchennyh sistem (u etoi, naprimer, tochno izvestno naklonenie orbity, rasstoyanie i tp.) eto samaya vysokaya massa. A imenno vysokie znacheniya mass ogranichivayut uravneniya sostoyaniya veshestva pri vysokoi plotnosti.


obzor arxiv:0801.1602 Pul'sarnye tumannosti v epohu Chandry (Pulsar Wind Nebulae in the Chandra Era)
Authors: O. Kargaltsev, G. G. Pavlov
Comments: 15 pages, 5 tables, 10 figures. To appear in the proceedings of "40 Years of Pulsars: Millisecond Pulsars, Magnetars, and More", August 12-17, 2007, McGill University, Montreal, Canada

V poslednie gody bol'shoe vnimanie specialistov privlekayut t.n. pul'sarnye tumannosti. Rabotayushii pul'sar daet potok chastic, kotorye vzaimodeistvuyut s okruzhayushim veshestvom. V itoge voznikaet specificheskoe obrazovanie. Blagodarya vysokomu uglovomu razresheniyu rentgenovskogo teleskopa Chandra udaetsya izuchat' mnogie iz etih tumannostei v melkih podrobnostyah. Krome togo, razvitie nazemnoi gamma-astronomii (H.E.S.S., MAGIC, ...) daet vozmozhnost' nablyudat' eti ob'ekty na TeVnyh energiyah. T.e., idet bol'shoi potok dannyh, nu i teoretiki ne sidyat, slozhiv v ruki. Tak chto est' chto obozret', chto avtory i delayut.

Est' krasivye kartinki.


Vypusk 176. 20 dekabrya 2007-09 yanvarya 2008 goda

arxiv:0712.3070 Vzryvy sverhnovyh i rozhdenie neitronnyh zvezd (Supernova explosions and the birth of neutron stars)
Authors: H.-Th. Janka, A. Marek, B. Mueller, L. Scheck
Comments: 10 pages, 8 figures, 19 ps files; to be published in Proc. of Conf. "40 Years of Pulsars: Millisecond Pulsars, Magnetars, and More", August 12-17, 2007, McGill Univ., Montreal, Canada;

Za gromkim nazvaniem skryvaetsya ne obzor obshirneishei tematiki ili predstavlenie istiny v poslednei instancii, a podrobnyi rasskaz o novyh rezul'tatah, poluchennyh avtorami pri chislennom modelirovanii vzryvov sverhnovyh. Novaya versiya programmy pozvolila obnaruzhit' razvitie eshe odnoi gidrodinamicheskoi neustoichivosti, a takzhe pozvolila luchshe izuchit' vozniknovenie vozmushenii v yadre i na poverhnosti novorozhdennoi neitronnoi zvezdy.


arxiv:0712.3212 Taiming blizkoi neitronnoi zvezdy RX J1856.5-3754 (Timing the Nearby Isolated Neutron Star RX J1856.5-3754)
Authors: M. H. van Kerkwijk, D. L. Kaplan
Comments: 4 pages, 2 figures, 2 tables; accepted for publication in Astrophysical Journal (Letters)

Eto blizhaishaya iz izvestnyh neitronnyh zvezd, odin iz ob'ektov Velikolepnoi semerki. Ee period - okolo 7 sekund. Teper' zhe udalos' tochno pomerit' i proizvodnuyu perioda. Esli iz nee poluchit' ocenku magnitnogo polya po magnito-dipol'noi formule, to vyidet 1.5 1013 Gs. Eto normal'no dlya ob'ektov Semerki. Odnako harakteristicheskii vozrast okazyvaetsya 4 milliona let, chto namnogo bol'she i ocenki po ostyvaniyu, i kinematicheskogo vozrasta. Znachit, nachal'nyi period dolzhen byl byt' dostatochno bol'shim (ili magnito-dipol'naya formula neprimenima). Krome togo, okazyvaetsya, chto magnito-dipol'naya svetimost' namnogo nizhe energetiki nablyudaemoi u etoi zvezdy tumannosti.


arxiv:0712.3826 Massivnaya neitronnaya zvezda v sharovom skoplenii M5 (A Massive Neutron Star in the Globular Cluster M5)
Authors: Paulo C. C. Freire, Alex Wolszczan, Maureen van den Berg, Jason W. T. Hessels
Comments: 23 pages in referee's format, 2 tables, 5 figures. Submitted to ApJ

Esli etot rezul'tat vystoit, to eto odno iz vazhneishih otkrytii 2007 goda. Ya uzhe pisal v obzorah o dannom pul'sare PSR B1516+02B, kogda avtory vykladyvali predvaritel'nye rezul'taty, napravlennye v materialy konferencii. Sut' v tom, chto, vozmozhno, otkryta ochen' massivnaya neitronnaya zvezda. Razumeetsya, kak eto vsegda i byvaet, avtory poluchayut nekotoroe raspredelenie veroyatnosti togo, chto massa neitronnoi zvezdy lezhit v kakih-to predelah. Tak vot, s veroyatnost'yu 95 procentov massa vyshe 1.6 solnechnyh mass. Skoree vsego, massa blizhe k 1.9 mass Solnca. Esli eto tak, to eto ochen' vazhno dlya teorii vnutrennego stroeniya etih ob'ektov. No etim delo ne ogranichivaetsya, poskol'ku ogranicheniya na teorii vnutrennego stroeniya neitronnyh zvezd avtomaticheski dayut vazhnuyu informaciyu dlya fundamental'nyh teorii v KHD.


arxiv:0712.4186 Aktivnost' kandidata v magnitary 4U 0142+61: vspleski i emissionnye linii (Activity from Magnetar Candidate 4U 0142+61: Bursts and Emission Lines)
Authors: Fotis P. Gavriil, Rim. Dib, Victoria M. Kaspi
Comments: To appear in the proceedings of the "40 Years of Pulsars: Millisecond Pulsars, Magnetars and More" conference, held 12-17 August 2007, in Montreal QC (AIP, in press, eds: C. Bassa, Z. Wang, A. Cumming, V. Kaspi)

Avtory rasskazyvayut o nablyudeniyah novogo perioda aktivnosti anomal'nogo rentgenovskogo pul'sara 4U 0142+61. Vazhno, chto v odnoi iz vspyshek u pul'sara obnaruzheny spektral'nye detali. Esli samuyu sil'nuyu iz linii interpretirovat' kak protonnuyu ciklotronnuyu liniyu, to poluchaetsya magnitarnoe pole, kotoroe u etogo ob'ekta i ozhidayut naiti.

O nedavnih infrakrasnyh nablyudeniyah magnitarov mozhno prochest' tut arxiv:0712.4171.


miniobzor arxiv:0801.0953 Zagadochnye slabye akkreciruyushie neitronnye zvezdy v nashei Galaktike (Enigmatic sub-luminous accreting neutron stars in our Galaxy)
Authors: Rudy Wijnands
Comments: 6 pages, Conference proceedings from 'A Population Explosion: The Nature and Evolution of X-ray Binaries in Diverse Environments', 28 Oct - 2 Nov, St. Petersburg Beach, FL

Razvitie tehniki nablyudenii v rentgenovskom diapazone pozvolyaet detal'no izuchat' dostatochno slabye istochniki v dvoinyh sistemah so svetimost'yu poryadka 1035 erg/s. Sredi nih est' i sil'no peremennye istochniki, i ob'ekty s dostatochno stabil'noi svetimost'yu. Po-vidimomu, bol'shinstvo yavlyaetsya neitronnymi zvezdami. Nekotorye iz nih mogut yavlyat'sya praroditelyami millisekundnyh radiopul'sarov. Etot poslednii moment delaet takie sistemy osobenno interesnymi. Krome togo, v nekotoryh sluchayah my mozhem poluchat' informaciyu o vnutrennem stroenii neitronnyh zvezd, esli nablyudaetsya teplovoe izluchenie, svyazannoe ne s akkreciei, a s zapasennym teplom i piknoyadernymi reakciyami.


arxiv:0801.1142 Tochnoe sobstvennoe dvizheniya pul'sara v Krabe i trudnosti vyyavleniya ugla mezhdu skorost'yu i os'yu vrasheniya u molodyh neitronnyh zvezd (A Precise Proper Motion for the Crab Pulsar, and the Difficulty of Testing Spin-Kick Alignment for Young Neutron Stars)
Authors: D. L. Kaplan, S. Chatterjee, B. M. Gaensler, J. Anderson
Comments: 15 pages, 6 figures. Accepted for publication in ApJ

V poslednie gody aktivno obsuzhdaetsya takaya velichina kak ugol mezhdu vektorom skorosti i os'yu vrasheniya neitronnoi zvezdy. Dlya nekotoryh odinochnyh radiopul'sarov udaetsya iz nablyudenii ocenit' etu velichinu, prichem v neskol'kih sluchayah znachenie polucheno s otnositel'no nebol'shimi oshibkami.

Pochemu eto vazhno? Okazalos', chto est' tendenciya k tomu, chto ugol nevelik, no pri etom i ne raven nulyu. Potencial'no eto mozhet dat' vazhnuyu informaciyu o mehanizme razgona neitronnyh zvezd (napomnyu, chto mnogie pul'sary imeyut ochen' vysokie prostranstvennye skorosti - do neskol'kih tysyach km v sek). A mehanizm etot, razumeetsya, zavyazan na mehanizm sverhnovoi. T.o., ugol mezhdu vektorami skorosti i sobstvennogo vrasheniya yavlyaetsya otpechatkom vzryva sverhnovoi. No ne tol'ko sverhnovoi! Ved' zvezda-praroditel' dvigalas' i vrashalas' i do vzryva. Bolee togo, ona mogla vhodit' v sostav tesnoi dvoinoi sistemy, t.e. mogla imet' vysokuyu orbital'nuyu skorost'. Eto, konechno, oslozhnyaet situaciyu.

Avtory privodyat novuyu ocenku ugla mezhdu napravleniem skorosti i sobstvennogo vrasheniya dlya pul'sara v Krabe i obsuzhdayut, chto moglo byt' prichinoi togo, chto ugol etot hotya i mal (menee 20 gradusov), no tem ne menee ne raven nulyu.


obzor arxiv:0801.1143 Blizkie neitronnye zvezdy s teplovym spektrom (Nearby, Thermally Emitting Neutron Stars)
Authors: D. L. Kaplan
Comments: 9 pages, one table, 3 figures. To appear in the proceedings of "40 Years of Pulsars: Millisecond Pulsars, Magnetars, and More", August 12-17, 2007, McGill University, Montreal, Canada

Dostatochno polnyi obzor po Velikolepnoi semerke i rodstvennym ob'ektam. Krome svodki nablyudatel'nyh dannyh avtor privodit rassuzhdeniya o tom, chem eti ob'ekty polezny dlya fiziki i astrofiziki i obsuzhdaet nereshennye voprosy.


Vypusk 175. 14-19 dekabrya 2007

arxiv:0712.2162 Relyativistskie modeli magnitarov: struktura i deformacii (Relativistic models of magnetars: structure and deformations)
Authors: A. Colaiuda, V. Ferrari, L. Gualtieri, J.A. Pons
Comments: 25 pages, 9 figures, submitted to MNRAS

Avtory rassmatrivayut, kak magnitnye polya razlichnoi konfiguracii deformiruyut neitronnye zvezdy. Konechno, mnogie parametry izvestny ploho (topologiya polya, ego raspredelenie vnutri zvezdy), poetomu raschety v sushestvennoi stepeni model'nye.

Dlya nablyudaemyh magnitarov (u nih dlinnye periody vrasheniya) iskazheniya formy za schet magnitnogo polya sil'nee, chem za schet vrasheniya. Eto vazhno dlya evolyucii etih ob'ektov (naprimer, mozhet izmenyat'sya ugol mezhdu magnitnoi os'yu i os'yu vrasheniya) i izlucheniya imi gravitacionnyh voln. A vot pri periodah poryadka desyatyh dolei sekundy dazhe magnitarnye polya dayut iskazhenie slabee, chem vrashenie. Pravda, vazhno, chto iskazheniya eti raznye. Vrashenie tol'ko splyushivaet zvezdu vdol' osi vrasheniya. A pole v zavisimosti ot topologii mozhet davat' prakticheski lyubye iskazheniya formy.


miniobzor arxiv:0712.2209 Central'nye kompaktnye ob'ekty v ostatakah sverhnovyh (Central Compact Objects in Supernova Remnants)
Authors: Andrea De Luca
Comments: 9 pages. Invited talk at the conference "40 Years of Pulsars: Millisecond Pulsars, Magnetars and More", August 12-17, 2007, Montreal (CA). To appear in the proceedings, ed. by C.Bassa, Z.Wang, A.Cumming and V.Kaspi, AIP, in press

Nebol'shoi obzor poslednih rezul'tatov po kompaktnym rentgenovskim istochnikam v ostatkah sverhnovyh. Napomnyu sut' problemy. Seichas my vidim v ostatkah okolo desyatka istochnikov, kotorye navernyaka (v nekotoryh sluchayah "pochti navernyaka") yavlyayutsya neitronnym zvezdami. Desyatok - eto ne malo. Radiopul'sarov, nadezhno associirovannyh s ostatkami primerno stol'ko zhe. Tak vot, kompaktnye istochniki eti na radiopul'sary sovsem ne pohozhi. T.e., kak minimum polovina neitronnyh zvezd dolzhna rozhdat'sya "inymi". Andrea privodit novye nablyudatel'nye rezul'taty i obsuzhdaet razlichnye gipotezy, vyskazannye po povodu etih rezul'tatov. Osobenno detal'no opisyvayutsya dannye po istochniku v ostatke RCW 103 i istochniku 1E 1207.


arxiv:0712.2460 Modelirovanie sliyanii chernyh dyr i neitronnyh zvezd s polnym uchetom effektov OTO (Fully General Relativistic Simulations of Black Hole-Neutron Star Mergers)
Authors: Zachariah B. Etienne et al.
Comments: 22 pages, 14 figures, submitted to Phys.Rev.D

Avtory predstavlyayut rezul'taty chislennogo modelirovaniya sliyaniya chernoi dyry i neitronnoi zvezdy, poluchennye s pomosh'yu novogo koda. Napomnyu, chto takie sobytiya vo-pervyh, sovershenno tochno yavlyayutsya moshneishimi istochnikami gravitacionnyh voln (i, skoree vsego, LIGO pervymi uvidit imenno ih), a vo-vtoryh, kakoe-to vremya takie sobytiya obsuzhdalis' kak istochniki korotkih gamma-vspleskov.

Rezul'taty podtverzhdayut, chto gamma-vsplesk sdelat' trudno, t.k. pochti vse veshestvo neitronnoi zvezdy srazu provalivaetsya v dyru, i lish' zhalkie procenty idut na obrazovanie diska. Razumeetsya, avtory rasschityvayut formu gravimpul'sa. Sravnenie rezul'tatov raschetov s dannymi o budushih "otlovlennyh" vspleskah gravizlucheniya pozvolit dat' vazhnye ogranicheniya na uravnenie sostoyaniya neitronnyh zvezd.


Vypusk 174. 01-13 dekabrya 2007

arxiv:0712.1040 Skol' bystro neitronnye zvezdy vrashayutsya pri rozhdenii? Ogranicheniya po arhivnym rentgenovskim nablyudeniyam vnegalakticheskih sverhnovyh (How rapidly do neutron stars spin at birth? Constraints from archival X-ray observations of extragalactic supernovae)
Authors: Rosalba Perna et al.
Comments: 12 pages, 2 figures, accepted for publication in MNRAS

My poka ploho znaem, kakimi rozhdayutsya neitronnye zvezdy: kakie u nih magnitnye polya, periody, massy, prostranstvennye skorosti. Ved' nablyudaem my uzhe proevolyucionirovavshie ob'ekty, da eshe vdobavok te, ktorye proshe uvidet' (naprimer, radio pul'sary). Vosstanovlenie nachal'nyh parametrov chashe vsego proishodit putem primeneniya populyacionnyh modelei. A hotelos' by bol'she pryamyh dannyh.

Avtory predlagayut ispol'zovat' rntgenovskie nablyudeniya sverhnovyh. Esli tam rodilas' neitronnaya zvezda, to my mozhem dat' ogranichenie na dopolnitel'noe energovydelenie, svyazannoe s kompaktnym ob'ektom. Energovydelenie zavisit ot vrasheniya i magnitnogo polya, znachit, my mozhem ogranichit' nekotoruyu kombinaciyu etih parametrov.

Razumeetsya, net neobhodimosti nablyudat' sverhnovuyu v moment vzryva. Bolee togo, togda tol'ko bystrovrashayushiesya magnitary mogut vnesti kakoi-to sushestvennyi vklad. Rech' idet ob issledovanii istoricheskih sverhnovyh (t.e., kogda vozrast tochno izvesten). Ispol'zovalis' nablyudeniya na sputnike Chandra.

Po mneniyu avtorov, oni mogut isklyuchit' dominirovanie sredi neitronnyh zvezd teh, chto rodilis' s ochen' korotkimi periodami. Konechno, dlya etogo im prishlos' zadat'sya neotorymi model'nymi predpolozheniyami (magnito-dipol'naya formula dlya energovydeleniya, nekotoroe raspredelenie po magnitnym polyam, izvestnoe po dannym o radiopul'sarah). Tem ne menee podhod interesnyi.

V zaklyuchenie otmechu, chto avtoram ne udalos' dat' ogranicheniya na nachal'nye periody magnitarov, poskol'ku te slishkom bystro zamedlyayutsya iz-za sverhsil'nyh magnitnyh polei. Tak chto k momentu nablyudenii vklad podobnyh obhektov v rentgenovskuyu svetimost' ostatka sverhnovoi byl by kraine mal.


arxiv:0712.1233 Korotkie gamma-vspleski s dlitel'nym izlucheniem iz-za zamedleniya protomagnitara (Short Duration Gamma-Ray Bursts with Extended Emission from Proto-Magnetar Spin-Down)
Authors: B.D. Metzger, E. Quataert, T.A. Thompson
Comments: 5 pages, 2 figures; submitted to MNRAS Letters

Dlya raznyh podvidov gamma-vspleskov prodozhayut predlagat' i razrabatyvat' raznye scenarii. Vse oni vklyuchayut v sebya obrazovanie kompaktnogo ob'ekta i diska vokrug nego, no detali razlichayutsya. Naprimer, est' korotkie vspleski, u kotoryh v dopolnenie k osnovnomu impul'su vidyat takzhe shirokii vsplesk dlitel'nost'yu do 100 sekund. V dannyh SWIFT takih nemalo. V etoi stat'e avtory razvivayut model', v kotoroi takie vspleski porozhdayutsya protomagnitarom, voznikshim ili pri kollapse belogo karlika, ili pri sliyanii belyh karlikov ili neitronnyh zvezd. Trebuyutsya dostatochno ekstremal'nye parametry: pole 3 1015 gauss pri periode 1 msek.


arxiv:0712.1353 Vliyanie magnitnogo polya na teplovuyu evolyuciyu neitronnyh zvezd (The impact of magnetic field on the thermal evolution of neutron stars)
Authors: Deborah N. Aguilera, Jose A. Pons, Juan A. Miralles
Comments: 4 pages, 3 figures, 1 table. Accepted for publication in APJ Letters

Dazhe esli nauchit'sya pravil'no schitat' vse processy ohlazhdeniya v sverhplotnom sverhtekuchem veshestve v nedrah neitronnoi zvezdy, to eto eshe ne znachit, chto my mozhem sravnivat' teoriyu i nablyudeniya. Vazhno takzhe pravil'no poschitat', chto budet proishodit' vo vneshnih sloyah, gde, vrode by, deistvuet kuda kak bolee ponyatnaya fizika. No ponyatnaya, ne oznachaet prostaya. Mnogie effekty poka uchityvayutsya ochen' ploho. Naprimer, vliyanie magnitnyh polei.

Teploprovodnost' vo vneshnih sloyah neitronnoi zvezdy svyazana s elektronami, a na nih magnitnoe pole ochen' dazhe vliyaet. Teploprovodnost' vdol' polya i poperek ochen' raznaya. Iz-za netrivial'noi konfiguracii magnitnogo polya temperatura poverhnosti neitronnoi zvezdy okazyvaet neodnorodnoi: na ekvatore holodnee, na polyuse - goryachee, esli my govorim o dipol'nom pole. No pole mozhet byt' nedipol'nym .... Krome togo, zatuhanie magnitnogo polya budet podogrevat' neitronnuyu zvezdy. V itoge, vse ochen' zaputano. Avtory s pomosh'yu dvumernyh raschetov pytayutsya hotya by chastichno razobrat'sya v etoi situacii.


arxiv:0712.1502 Gigantskaya vspyshka istochnika myagkih povtoryayushihsya gamma-vspleskov v Tumannosti Andromedy, M31 (A Giant Flare from a Soft Gamma Repeater in the Andromeda Galaxy, M31)
Authors: E.P. Mazets et al.
Comments: 15 pages, 5 figures, submitted to ApJ

V fevrale etogo goda pribory eksperimenta Konus-Vind, a takzhe drugie detektory, zafiksirovali korotkii zhestkii vsplesk. Po svoim svoistvam on ochen' pohozh na gigantskie vspyshki magnitarov. Prichem, vsplesk proeciruetsya na M31. T.o., vse govorit v pol'zu togo, chto eto vsplesk vnegalakticheskogo istochnika myagkih povtoryayushihsya gamma-vspleskov.


Vypusk 173. 20-30 noyabrya 2007

miniobzor arxiv:0711.3650 Proishozhdenie magnitnyh polei neitronnyh zvezd (Origin of neutron star magnetic fields)
Authors: H.C. Spruit
Comments: 8 pages, Review to appear in "40 years of pulsars", ed. A. Cumming, AIP

Magnitnye polya ili svyazany s usileniem polya pri kollapse (sohranyaetsya magnitnyi potok), ili generiruyutsya v protoneitronnyh zvezdah, t.e. prakticheski srazu posle kollapsa. V obzore osnovnoe vnimanie udeleno generacii polya, t.. tut mnogo interesnyh nereshennyh voprosov. Avtor rassmatrivaet vse processy bolee-menee "na pal'cah", t.e. stat'ya vpolne dostupna.


arxiv:0711.3780 Vsplesk 2-sekundnogo anomal'nogo rentgenovskogo pul'sara 1E 1547.0-5408 (Outburst of the 2 s Anomalous X-ray Pulsar 1E 1547.0-5408)
Authors: J.P. Halpern, E.V. Gotthelf, J. Reynolds, S.M. Ransom, F. Camilo
Comments: 7 pages, 5 figures, to appear in The Astrophysical Journal

1E 1547.0-5408 - interesnyi istochnik. On byl otkryt eshe v 1980 godu sputnikov Einshtein (o chem i govorit bukva E v nazvanie ob'ekta). Pozzhe on byl zapodozren kak anomal'nyi rentgenovskii pul'sar. Nedavno eto podozrenie podtverdilos'. Bolee togo, u istochnika byli otkryty radiopul'sacii s periodom 2 sekundy. Eto samyi korotkii period sredi vseh anomal'nyyh rentgenovskih pul'sarov. Na moi vzglyad, etot istochnik nachinaet razmyvat' granicu mezhdu pul'sarami i anomal'nymi rentgenovskimi pul'sarami.

V dannoi stat'e rassmotreny odnovremennye rentgenovskie i radio nablyudeniya istochnika. Avtory obnaruzhili ego v vysokom sostoyanii. T.e., istochnik stal moshnee. Ego goryachee pyatno rasshirilos'. Vazhno, chto radioizluchenie mozhet byt' svyazano s etoi povyshennoi aktivnost'yu. T.e., v istochnike proishodit "chto-to" (skoree vsego izmenenie konfiguracii magnitnogo polya), iz-za chego on stanovitsya goryachee, a krome togo, nachinaet izluchat' v radio.

Ssylka na katalog magnitarov.


miniobzor arxiv:0711.4278 Izuchenie gamma-pul'sarov s pomosh'yu GLAST (Gamma-Ray Pulsar Studies with GLAST)
Authors: D. J. Thompson
Comments: 8 pages, 5 figures. To appear in the proceedings of "40 Years of Pulsars: Millisecond Pulsars, Magnetars, and More", August 12-17, 2007, McGill University, Montreal, Canada

Ochen' tolkovyi obzor po gamma izlucheniyu radiopul'sarov i perspektivam ego issledovaniya na sputnike GLAST, kotoryi sovsem skoro dolzhen byt' zapushen.


Vypusk 172. 01-19 noyabrya 2007

arxiv:0711.0925 Vosem' novyh millisekundnyh pul'sarov v NGC 6440 i NGC 6441 (Eight New Millisecond Pulsars in NGC 6440 and NGC 6441)
Authors: Freire P.C.C. et al.
Comments: Submitted to the Astrophysical Journal, including referee's comments. 37 pages in referee's format, 6 tables, 7 figures

Posle togo, kak v sharovom skoplenii Terzan 5 bylo otkryto 30 millisekundnyh pul'sarov, narod ne mog ne brosit'sya iskat' v drugih. Delo tut dazhe ne tol'ko i i ne stol'ko v banal'nom uvelichenii chisla izvestnyh ob'ektov, a v tom, chtoby razobrat'sya s formirovaniem i evolyuciei etih ob'ektov, i, vozmozhno, natknut'sya na chto-nibud' interesnoe. Ne isklyucheno, chto natknulis'.

Sredi vos'mi novyh pul'sarov (pyat' v NGC 6440 i tri v NGC 6441) est' ochen' i ochen' lyubopytnye. Napomnyu, chto millisekundnymi pul'sary stanovyatsya v dvoinyh sistemah, kogda na nih akkreciruet veshestvo zvezdy-sosedki. Pri etom ne tol'ko chastota vrasheniya uvelichivaetsya, no i massa, estestvenno, vozrastaet. Poetomu mozhno nadeyat'sya naiti ochen' massivnuyu neitronnuyu zvezdu. Eto vazhno, tak kak pozvolyaet dat' zhestkie ogranicheniya na fiziku pri sverhvysokih plotnostyah (tipa 10 yadernyh). Odin iz vos'mi pul'sarov, po ocenke avtorov, imeet massu 2.74 plyus-minus 0.21 (eto odno standartnoe otklonenie). Esli rezul'tat podtverditsya (napomnyu, chto rekordnaya, do nedavnego vremeni, massa taki ``rassosalas'`` - novye nablyudeniya ne podtverdili prezhnee znachenie), to eto budet kraine vazhnym (naprimer, budut zakryty sushestvuyushie modeli kvarkovyh zvezd).

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


arxiv:0711.1880 PSR J1738+0333: novaya gravitacionnaya laboratoriya (PSR J1738+0333: a new gravitational laboratory)
Authors: Paulo C. C. Freire, Bryan A. Jacoby, Matthew Bailes
Comments: 3 pages, 2 figures. To appear in the proceedings of "40 Years of Pulsars: Millisecond Pulsars, Magnetars, and More", August 12-17, 2007, McGill University, Montreal, Canada

Kratko opisany nablyudeniya novogo interesnogo dvoinogo pul'sara. Sputnikom neitronnoi zvezdy yavlyaetsya malomassivnyi belyi karlik. Sistema interesna tem, chto obladaet rekordno nizkim ekscentrisitetom - menee 10-7. Poka, pravda, tochnost' nablyudenii ne ochen' vysoka - nado prosto nablyudat' dol'she. Esli stol' nizkoe znachenie ekscentrisiteta podtverditsya, to eto sdelaet dannuyu sistemu interesnym instrumentom dlya izucheniya gravitacii.

Sm. Takzhe dve drugie stat'i etoi gruppy: arxiv:0711.1883 i arxiv:0711.2028.


miniobzor arxiv:0711.2579 Ogranicheniya na uravnenie sostoyaniya neitronnyh zvezd po malomassivnym rentgenovskim dvoinym v spokoinom sostoyanii (Constraining the neutron star equation of state using quiescent low-mass X-ray binaries)
Authors: P.G. Jonker
Comments: 7 pages, 3 figures, proceedings "40 years of pulsars" conference

Dlya polucheniya ogranichenii na modeli vnutrennego stroeniya neitronnyh zvezd ispol'zuyutsya opredeleniya mass i radiusov neitronnyh zvezd, a takzhe vydelenie massivnyh ob'ektov (t.k. dlya raznyh uravneniei sostoyaniya verhnie predely na massu razlichny, a potomu obnaruzhenie dazhe odnoi ochen' massivnoi neitronnoi zvezdy razom perecherkivaet bol'shuyu gruppu t.n. myagkih uravnenii sostoyaniya). Vse eto mozhno delat', provodya detal'nye issledovaniya malomassivnyh rentgenovskih dvoinyh v spokoinom sostoyanii.

"Spokoinoe" oznachaet. Chto net akkrecii, i zvezda svetit za schet zapasennogo tepla i piknoyadernyh reakcii. Dlya mnogih istochnikov neploho izvestny rasstoyaniya (osobenno, esli dvoinaya nahoditsya v sharovom skoplenii), poetomu mozhno delat' horoshie ocenki radiusa. Dvoistvennost' pozvolyaet ocenivat' massu. Ochen' bystroe ohlazhdenie govorit o nalichii pryamogo URKA processa. On vozmozhen tol'ko pri dostatochno bol'shih plotnostyah, kotorye ne dlya vseh uravnenii sostoyaniya dostupny.

Vse eto i obozrevaetsya v obzore.

Poputno otmechu obzor po strannym zvezdam arxiv:0711.2639.


Vypusk 171. 17-31 oktyabrya 2007

obzor arxiv:0710.3517 Pul'sarnoe izluchenie vysokih energii v modeli polyarnoi shapki i Slot Gap (Pulsar High-Energy Emission From the Polar Cap and Slot Gap)
Authors: Alice K. Harding
Comments: 23 pages, 8 Figures, Invited Review at 363-Heraeus-Seminar on Neutron Stars and Pulsars, ed. W. Becker

Kak izvestno, detali mehanizma izlucheniya pul'sarov ostayutsya neizvestnymi. V chastnosti, neyasno gde (blizko k neitronnoi zvezde, okolo svetovogo cilindra, ili zhe gde-to poseredine) rozhdayutsya zhestkie kvanty, ispuskaemye etimi neitronnymi zvezdami. V dannom obzore rassmotreny dve modeli.

V pervoi modeli uskorenie chastic proishodit v polyarnom zazore - t.e. dostatochno blizko k poverhnosti neitronnoi zvezdy. Vo vtoroi, zazor predstavlyaet soboi uzkuyu rasshelinu (Slot) vblizi poslednih otkrytyh silovyh linii (dobavlyu, chto est' eshe tret'ya model' - vneshnego zazora - rassmatrivaemaya v otdel'noi stat'e). Mozhno nadeyat'sya, chto v samom nedalekom budushem rezul'taty so sputnika GLAST pozvolyat sdelat' vybor mezhdu modelyami.


miniobzor arxiv:0710.3626 Dvadcat' let poiskov (i nahodok) pul'sarov v sharovyh skopleniyah (Twenty Years of Searching for (and Finding) Globular Cluster Pulsars)
Authors: Scott M. Ransom
Comments: 9 pages, 6 figures. Submitted review for the "40 Years of Pulsars" conference in Montreal, Aug 2007. To be published by the AIP

V sharovyh skopleniyah slozhilis' osobenno blagopriyatnye usloviya dlya formirovaniya nekotoryh tipov dvoinyh sistem. V chastnosti, tam mnogo dvoinyh millisekundnyh pul'sarov. Poisku i otkrytiyam razlichnyh predstavitelei etogo semeistva i posvyashen nebol'shoi obzor. Naideno nemalo interesnogo. Naprimer, pul'sar s rekordno korotkim periodom vrasheniya naiden imenno v sharovom skoplenii.


miniobzor arxiv:0710.5026 Parksovskii nabor pul'sarov dlya taiminga (The Parkes Pulsar Timing Array)
Authors: R. N. Manchester
Comments: 9 pages, 6 figures, Proceedings of "40 Years of Pulsars: Millisecond Pulsars, Magnetars and More", Montreal, August 2007

Pul'sary "chuvstvuyut" gravitacionnye volny. Buduchi tochnymi chasami, oni "sbivayutsya", kogda prohodit gravvolna (krome togo, sboi budet nablyudat'sya i togda, kogda volna prohodit cherez Zemlyu). Poetomu, nablyudaya neskol'ko pul'sarov s horosho izvestnym taimingom, mozhno dat' ogranicheniya na gravvolny. T.e., pul'sary rabotayut kak gravitacionnye detektory. PPTA (Parkes Pulsar Timing Array) - eto kak raz nabor iz 20 ob'ektov dlya podobnyh issledovanii. Provodyatsya regulyarnye nablyudeniya etih pul'sarov, chto i pozvolyaet delat' vsyakie interesnye vyvody po povodu gravvoln (i ne tol'ko gravvoln, kstati). Poka, konechno, rech' idet tol'ko o verhnih predelah, no ved' i detektory poka nikakogo polozhitel'nogo rezul'tata v registracii gravsignala ne dali :)


miniobzor arxiv:0710.5374 Vklad Kosmicheskogo teleskopa v izuchenie neitronnyh zvezd (The HST contribution to neutron star astronomy)
Authors: R.P. Mignani
Comments: 4 pages, to be published in Proc. of 41st ESLAB Symposium: The Impact of HST on European Astronomy

V korotkom obzore Roberto Min'yani rasskazyvaet, kakuyu rol' sygrali nablyudeniya na habblovskom teleskope v astronomii neitronnyh zvezd.

Neitronnye zvezdy yavlyayutsya ochen' slabymi istochnikami v opticheskom diapazone (za isklyucheniem pul'sarov v Krabe i Parusah, kotorye i byli prakticheski edinstvennymi horosho izuchennymi v optike neitronnymi zvezdami do zapuska Kosmicheskogo teleskopa). Poetomu neudivitel'no, chto ni o kakih massovyh otozhdestvleniyah etih ob'ektov s pomosh'yu nazemnyh teleskopov v 80-h godah i ranee ne bylo i rechi. S zapuskom Habbla situaciya rezko izmenilas': chislo otozhdestvlennyh v optike neitronnyh zvezd perevalilo za desyatok. Krome klassicheskih radiopul'sarov v optike nablyudayut Gemingu i nekotorye iz ob'ektov, vhodyashih v Velikolepnuyu semerku.

O poiskah novyh kandidatov v ostyvayushie neitronnye zvezdy (tipa Velikolepnoi semerki) mozhno prochest' zdes': arxiv:0710.5192


Vypusk 170. 01-16 oktyabrya 2007

obzor arxiv:0709.4635 Cvetnaya sverhprovodimost' v plotnom kvarkovom veshestve (Color superconductivity in dense quark matter)
Authors: Mark G. Alford, Krishna Rajagopal, Thomas Schaefer, Andreas Schmitt
Comments: 62 pages, submitted to Reviews of Modern Physics

Bol'shoi obzor, posvyashennyi sverhprovodimosti v kvarkovom veshestve. Razumeetsya, v pervuyu ochered' takaya situaciya vozmozhna v nedrah kompatnyh zvezd (nazvat' ih "neitronnymi" v dannom sluchae uzhe nel'zya). Obzor ochen' detal'nyi, no inteersen, skoree vsego, tol'ko specialistam (za isklyucheniem vvedeniya i zaklyuchitel'noi, "astrofizicheskoi" chasti).


miniobzor arxiv:0710.0397 Teoriya pul'sarnyh tumannostei (Theory of Pulsar Wind Nebulae)
Authors: N. Bucciantini
Comments: 9 page, 5 figures, Proceeding of the conference "40 Years of Pulsars", 12-17 August 2007, Montreal, Canada. (figures are not properly displayed in .ps or .pdf version please download archive for them)

Ne vse pomnyat, chto Krabovidnaya tumannost' ne est' ostatok sverhnovoi v strogom smysle etogo slova. Eto t.n. plerion. Inache govorya - pul'sarnaya tumannost' (PWN). V poslednie gody v issledovaniyah PWN byl dostignut sushestvennyi progress. Dannye s Habbla, Chandry i HMM-N'yutona dali vozmozhnost' ne tol'ko detal'no izuchat' morfologiyu etih obrazovanii, no i sledit' za ih dinamikoi. Razumeetsya, tut zhe podtyanulis' teoretiki i specialisty po chislennomu modelirovaniyu. V itoge - est' chto obozrevat', chto i delaet avtor v svoei stat'e.


arxiv:0710.0675 Poisk pul'sarov na LOFAR (Finding pulsars with LOFAR)
Authors: Joeri van Leeuwen, Ben Stappers
Comments: 3 pages, Proceedings of "40 Years of Pulsars: Millisecond Pulsars, Magnetars, and More" (12-17 August 2007 at McGill, Montreal Canada)

Po suti, predstavlen populyacionnyi sintez radiopul'sarov dlya opredeleniya togo, chto smozhet uvidet' sistema teleskopov LOFAR, nachinayushaya rabotat' v sleduyushem godu.

Dlya blizkih slabyh pul'sarov mozhno ozhidat' nekotorgo proryva (krome togo, polagayu, oni smogut uvidet' Velikolepnuyu Semerku, ili postavit' OChEN' zhestkie predely, takzhe ochen' vazhno otnablyudat' Calvera).

Takzhe avtory obsuzhdayut nablyudenie pul'sarov v drugih galaktikah. V predelah odnogo megaparseka (ili dazhe chut' dal'she) mozhno ozhidat' otkrytie samyh yarkih pul'sarov.


arxiv:0710.1745 Obzor GBT350 po poisku radiopul'sarov i tranzientov v severnoi chasti galakticheskoi ploskosti (The GBT350 Survey of the Northern Galactic Plane for Radio Pulsars and Transients)
Authors: J.W.T. Hessels et al.
Comments: To appear in the proceedings of "Forty Years of Pulsars: Millisecond Pulsars, Magnetars and More" held in Montreal, Canada, August 12-17, 2007. 3 pages, 2 figures

Avtory predstavlyayut predvaritel'nye rezul'taty po poisku novyh pul'sarov. Obzor provodilsya na teleskope GBT na chastote 350 Mgc. Novyi obzor bolee chuvstvitelen k millisekundnym i dolgoperiodicheskim pul'saram, chem ego predshestvenniki (v etoi oblasti). Obnaruzheno 33 novyh pul'sara. Nekotorye iz nih imeyut dostatochno interesnye svoistva.


arxiv:0710.1788 Zhestkii verhnii predel na pul'siruyushee radio izluchenie ot kompaktnogo ob'ekta 1RXS J141256.0+792204 (A Strong Upper Limit on the Pulsed Radio Luminosity of the Compact Object 1RXS J141256.0+792204)
Authors: J.W.T. Hessels et al.
Comments: To appear in A&A. 3 pages

Postavlen ochen' zhestkii verhnii predel na radioizluchenie Kal'very (Calvera). Ya nachinayu verit' v to, chto nasha iznachal'naya dogadka, chto eto v samom dele ob'ekt tipa Velikolepnoi semerki, no porozhdennyi vysokoskorostnoi zvezdoi, verna. Esli skorost' zvezdy-praroditelya byla poryadka 100-200 km/s, chto vpolne vozmozhno dlya "ubegayushei zvezdy" (runaway star), to neitronnaya zvezda mogla "vylupit'sya" uzhe ochen' vysoko nad ploskost'yu Galaktiki.


miniobzor arxiv:0710.2047 Teoriya i nablyudeniya ostyvayushih neitronnyh zvezd (Theory of cooling neutron stars versus observations)
Authors: D. G. Yakovlev et al.
Comments: 9 pages, 4 figures, 3 tables, to appear in the proceedings of "40 Years of Pulsars" held in Montreal, Canada, August 12-17, 2007, eds. C. Bassa, Z. Wang, A. Cumming, V. Kaspi, AIP, submitted

Poskol'ku ostyvaniem neitronnyh zvezd seichas zanimaetsya neskol'ko grupp teoretikov, a potok nablyudenii rastet, obzorov po etoi tematike poyavlyaetsya ne malo. Tem ne menee, v dannom sluchae my imeem otlichnyi primer togo, kak v dostatochno ogranichennyi ob'em mozhno vmestit' vse samoe glavnoe i pro teoriyu, i pro nablyudeniya, da eshe i s kartinkami!


arxiv:0710.2056 Vrashayushiesya radiotranzienty: rentgenovskie nablyudeniya (Rotating Radio Transients: X-ray observations)
Authors: Nanda Rea
Comments: 8 pages, 4 figures; review at the conference "Astrophysics of Compact Objects", China

Opisany rezul'taty rentgenovskih nablyudenii treh RRATs - Rotating Radio Transients. Odin iz etih ob'ektov byl sluchaino "zasnyat" Chandroi, v stat'e predstavleny rezul'taty posleduyushih bolee detal'nyh nablyudenii. RRATs vydelyayutsya svoimi moshnymi ochen' korotkimi impul'sami. Tak vot, rentgenovskie dannye pokazali, chto pul'sy prihodyat tochno v moment maksimuma rentgenovskoi krivoi bleska.

Dlya dvuh drugih RRATS, kotorye takzhe pytalis' nablyudat' v rentgene, polucheny lish' verhnie predely. Prichem predely ne slishkom zhestkie, tak chto nuzhno nablyudat' s bol'shimi ekspoziciyami.

Poka neyasno to li RRATs - eto osobaya gruppa neitronnyh zvezd, to li eto takoi "podvid" radiopul'sarov, ch'i nablyudatel'nye proyavleniya svyazany ne s fizikoi, a prosto s ih orientaciei otnositel'no nas i dostatochno bol'shim rasstoyaniem, to li RRATs - eto neodnorodnaya gruppa istochnikov, kotorye ob'edinyaet lish' nalichie millisekundnyh impul'sov.


miniobzor arxiv:0710.2475 Bystrye rentgenovskie oscillyacii vo vremya vspyshek magnitarov (Fast X-ray Oscillations During Magnetar Flares)
Authors: Tod E. Strohmayer
Comments: 8 pages, 3 figures, conference proceedings, "Astrophysics of Compact Objects," 2007, Huangshan, China

Nekotoroe vremya nazad analiz "pul'siruyushego hvosta" vspyshki, nablyudavsheisya 27 dekabrya 2004 goda ot odnogo iz istochnikov myagkih povtoryayushihsya gamma-vspleskov, pokazal nalichie kvaziperiodicheskih oscillyacii na neskol'kih chastotah poryadka desyatkov gerc i vyshe. Posle etogo byla provedena pereobrabotka analogichnyh dannyh po vspyshke 27 avgusta 1998 goda. Tam byli obnaruzheny analogichnye oscillyacii. V stat'e dan obzor dannyh po etomu yavleniyu, a takzhe obsuzhdayutsya vozmozhnye ob'yasneniya. Skoree vsego, my imeem delo s torsionnymi kolebaniyami neitronnoi zvezdy.


arxiv:0710.2793 Roscherk magnitara SGR 1806-20 na magnitnom pole Zemli (The SGR 1806-20 magnetar signature on the Earth's magnetic field)
Authors: Mioara Mandea, Georgios Balasis
Comments: Geophys. J. Int., 167, 2006

Vspyshka istochnika myagkih povtoryayushihsya gamma-vspleskom SGR 1806-20, proizoshedshaya 27 dekabrya 2004 goda, nadelala shuma. V chastnosti, ona okazala sushestvennoe vliyanie na sostoyanie zemnyh okrestnostei: izmenila ionizaciyu, vozmutila magnitnoe pole. Vot pro poslednee-to i rasskazyvaetsya v stat'e.

Avtory analiziruyut dannye sputnika CHAMP. Soglasno ih rezul'tatam v povedenii zemnogo magnitnogo polya nablyudalas' periodichnost' s periodom 7.5 sekund - t.e. s periodom vrasheniya magnitara.

O povedenii samogo "vinovnika" spustya dva goda posle vspyshki mozhno prochest' zdes'.

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


Vypusk 169. 19-30 sentyabrya 2007

arxiv:0709.4094 Vyyavlenie svyazi mezhdu moshnymi pul'sarami i ochen' vysokoenergichnymi gamma-istochnikami (Establishing a connection between high-power pulsars and very-high-energy gamma-ray sources)
Authors: S. Carrigan et al., for the H.E.S.S. Collaboration
Comments: 4 pages, Proceedings of the 30th ICRC, Merida, Mexico

Interesnaya rabota (a zaodno ob'edinyu tut raznye stat'i H.E.S.S. dlya materialov 30th ICRC).

Avtory predstavlyayut rezul'taty sistematicheskogo issledovaniya pul'sarov v TeVnom diapazone. Sdelano eto na osnove obzora vnutrennei Galaktiki na H.E.S.S. V etu oblast' popalo 435 pul'sarov. Avtory pokazyvayut, chto moshnye pul'sary (obychno eto molodye ob'ety, u nih temp vydeleniya vrashatel'noi energii ochen' velik) ochen' chasto nablyudayutsya kak istochniki zhestkogo gamma. Iz 435 H.E.S.S. uvidel 30. Eto mnogo dazhe s uchetom togo, chto avtory ne isklyuchayut, chto chast' iz etih 30 mozhet okazat'sya sluchainym sovpadeniem. Vozmozhno, eto samaya mnogochislennaya populyaciya TeVnyh istochnikov v Galaktike.

O drugih rabotah po H.E.S.S. V arxiv:0709.4103 rasskazyvaetsya o nablyudeniyah ostatka sverhnovoi RCW 86. V arxiv:0709.4103 opisano otkrytie kandidata v pul'sarnye tumannosti - istochnika HESS J1718-385. Dlya nekotoryh ob'ektov H.E.S.S. daet tol'ko verhnie predely. Svodka takovyh dlya aktivnyh yader galaktik dana v stat'e arxiv:0709.4598. A vot galaktika PG 1553+113 byla obnaruzheno, chto i opisano v arxiv:0709.4602. Vspyshka aktivnogo yadra PKS 2155-304 opisana v rabote arxiv:0709.4608. Avtory utverzhdayut, chto vspyshka dostatochno neobychna. Nakonec, stat'ya arxiv:0709.4621 posvyashena nablyudeniyam ostatka sverhnovoi RX J0852.0-4622.
Ob otkrytii ocherednoi lacertidy i ogranicheniyah na vnegalakticheskoe fonovoe izluchenie mozhno prochest' v arxiv:0709.4584 (eto uzhe ne materialy konferencii, a original'naya stat'ya).


arxiv:0709.4526 Issledovanie proishozhdeniya magnitnogo polya neitronnyh zvezd: magnitnye svoistva OV-zvezd-praroditelei (Exploring the origin of neutron star magnetic field: magnetic properties of the progenitor OB stars)
Authors: V. Petit, G.A. Wade, L. Drissen, T. Montmerle
Comments: 5 pages, 4 figures 40 Years of Pulsars conference: Millisecond Pulsars, Magnetars and More. McGill University, Montreal, Canada, August 12-17, 2007.

Proishozhdenie magnitnyh polei magnitarov ostaetsya zagadkoi. To li oni generyatsya na stadii protoneitronnoi zvezdy, to li zvezdy-praroditeli sami byli sil'no zamagnicheny, tak chto posle kollapsa i kompaktnye ob'ekty okazalis' s superpolyami. Avtory issleduyut vtoruyu vozmozhnost', pytayas' izmerit' polya massivnyh OV-zvezd. Vyvod avtorov lyubopyten. Oni polagayut, chto vtoraya vozmozhnost' (kollaps sil'no zamagnichennyh zvezd) ne prohodit ne potomu, chto sil'no zamagnichennyh massivnyh zvezd malo, a potomu, chto ih mnogo! Iz vos'mi issledovannyh zvezd tri okazalis' s sil'nymi polyami.



Vypusk 167. 25 avgusta - 10 sentyabrya 2007

arxiv:0708.3615 Relyativistskie linii izlucheniya zheleza ot malomassivnyh rentgenovskih dvoinyh v roli izmeritelei radiusov neitronnyh zvezd (Relativistic iron emission lines in neutron star low-mass X-ray binaries as probes of neutron star radii)
Authors: Edward M. Cackett, et al.
Comments: 5 pages, 3 figures, 3 tables, submitted to ApJL

Avtory opisyvayut nablyudeniya na sputnike Suzaku. Cel'yu bylo issledovanie linii zheleza v spektrah malomassivnyh rentgenovskih dvoinyh. Izuchenie etih linii mozhet pozvolit' dat' sushestvennye ogranicheniya na radiusy neitronnyh zved. Ideya v tom, chtoby detal'no rassmotret' linii, ispuskaemye s vnutrennego kraya akkrecionnogo diska. Yasno, chto razmer neitronnyi zvezdy men'she. Poskol'ku dlya nekotoryh malomassivnyh rentgenovskih dvoinyh vnutrennii krai diska podbiraetsya ochen' blizko k poverhnosti kompaktnogo ob'ekta, mozhno postavit' horoshii verhnii predel na razmer neitronnoi zvezdy. Predely sootvetstvuyut radiusam poryadka 14.5-16.5 km, esli predpolozhit', chto massy neitronnyh zvezd ravny 1.4 solnechnyh.

Sm. takzhe arxiv:0708.3648, gde rech' idet o nablyudenii linii zheleza ot odnogo iz ob'ektov, popavshem v lenty novostei. I arxiv:0708.3816, gde primenyaetsya drugoi podhod dlya ogranicheniya razmerov i mass neitronnyh zvezd na osnove ih rentgenovskih spektrov.


arxiv:0708.4251 Ukazaniya na soosnost' vektorov uglovoi i prostranstvennoi skorosti u pul'sarov. II. Novye dannye i vysota izluchayushei oblasti (Evidence for alignment of the rotation and velocity vectors in pulsars. II. Further data and emission heights)
Authors: Simon Johnston, M. Kramer, A. Karastergiou, G. Hobbs, S. Ord, J. Wallman
Comments: Accepted by MNRAS. 14 pages

Avtory privodyat dannye po polyarizacionnym issledovaniyam 22 pul'sarov. Osnovnyh rezul'tatov dva. Vo-pervyh, dlya nekotoryh iz neitronnyh zvezd udalos' ocenit' ugol mezhdu os'yu vrasheniya i napravleniem prostranstvennoi skorosti. Vo-vtoryh, avtory smogli sdelat' ocenki vysoty nad poverhnost'yu neitronnoi zvezdy, na kotoroi ispuskaetsya izluchenie v raznyh fazah. Ugly ocenili dlya 14 pul'sarov. U semi iz nih oni dostatochno maly. Eto nahoditsya v soglasii s bolee rannimi rezul'tatami na men'shei statistike (hotya, ranee polagali, chto u vseh oni mogut byt' maly). Chto kasaetsya vysot izlucheniya, to, opyat' zhe v soglasii s bolee rannimi dannymi, chto izluchenie v seredine profilya impul'sa generiruetsya na bolee nizkih vysotah, chem po krayam profilya.


arxiv:0709.0061 GRB060602B = Swift J1749.4-2807: neobychnaya tranzientnaya dvoinaya s neitronnoi zvezdoi (GRB060602B = Swift J1749.4-2807: an unusual transiently accreting neutron-star X-ray binary)
Authors: Rudy Wijnands et al.
Comments: submitted to MNRAS

Pohozhe, chto odin iz gamma-vspleskov na samom dele yavlyaetsya neobychnoi vspyshkoi na neitronnoi zvezde v tesnoi dvoinoi sisteme. Avtory polagayut, chto ne isklyucheno, chto est' mnogo sistem takogo tipa, no poka oni uskol'zayut ot nablyudatelei iz-za trudnoulovimosti ih vspyshek.


Vypusk 166. 14-24 avgusta 2007

arxiv:0708.1792 Izluchayushaya kolonka i krivye bleska dvoinyh rentgenovskih pul'sarov (Radiative Column and Light Curve of X-Ray Binary Pulsars)
Authors: S. Karino
Comments: 13 pages, 7 figures, accepted for publication in PASJ

V teorii radiopul'sarov, gde voobshe mnogo belyh pyaten, est' vazhnyi nereshennyi vopros. Svyazan on s izmeneniem ugla mezhdu os'yu vrasheniya i os'yu magnitnogo dipolya. V modeli magnito-dipol'nyh poter' etot ugol umen'shaetsya (osi stremyatsya stat' parallel'nymi drug drugu). V modeli tokovyh poter' (Beskin, Gurevich, Istomin) - ugol stremitsya k 90 gradusam. Dannye po radiopul'saram ne dayut vozmozhnosti vybrat' mezhdu dvumya variantami. Nekotoroe vremya nazad mne stalo yasno, chto mogut pomoch' rentgenovskie pul'sary, osobenno v sistemah, gde kompan'onom yavlyaetsya massivnaya zvezda, a akkreciya idet iz zvezdnogo vetra. V takih sistemah proshlo malo vremeni s teh por, kak neitronnaya zvezda ushla so stadii ezhekcii. Krome togo, akkrecionnyi potok takov, chto sam on ne mozhet sushestvenno povliyat' na ugol. Znachit, izuchiv raspredelenie uglov dlya neitronnyh zvezd v takih sistemah, mozhno uznat', kakimi byli ugly na moment okonchaniya stadii ezhekcii. Odnako opredelit' ugol dlya rentgenovskogo pul'sara tozhe ne ochen' prosto. Dlya etogo nado postroit' dovol'no slozhnuyu model'. Imenno eto i sdelano avtorom predlagaemoi stat'i.

Avtor postroil model' izlucheniya rentgenovskogo pul'sara. Dlya 117 istochnikov polucheny ocenki uglov. Oni pokazyvayut, chto ugly neveliki. Avtor ne obsuzhdaet opisannyi vyshe aspekt - "eksgumaciyu" radiopul'sarov dlya opredeleniya povedeniya uglov na stadii ezhekcii. Odnako na moi vzglyad, rezul'taty svidedel'stvuyut v pol'zu togo, chto ugly ne stremyatsya k 90 gradusam. Pravda, eto ne oznachaet, chto model' tokovyh poter' neverna. Deistvitel'nost' neskol'ko slozhnee. Delo v tom, chto na vtoroi chasti stadii ezhekcii - stadii mertvogo radiopul'sara - ugol mozhet evolyucionirovat' v storonu umen'sheniya. No po krainei mere yasno, chto v itoge6 na moment okonchaniya stadii ezhekcii, ugly maly.


arxiv:0708.2372 Poisk pul'sara v ostatke SN1987A (Searching for a Pulsar in SN1987A)
Authors: R. N. Manchester
Comments: 10 pages, 3 figures. To appear in "Supernova 1987A: Twenty Years After: Supernovae and Gamma-Ray Bursters", edited by S. Immler, K. W. Weiler and R. McCray, American Institute of Physics, New York, 2007, in press

Opisany rannie i nedavnie poiski radiopul'sara (ili proyavlenii ego aktivnosti) na meste vzryva sverhnovoi 1987 g. v Bol'shom Magellanovom oblake. Rezul'taty vo vseh diapazonah otricatel'nye. Tem ne menee, eto poka nichemu ne protivorechit. Esli neitronnaya zvezda rodilas' s ne slishkom bol'shim magnitnym polem i ne slishkom korotkim periodom (a poslednie dannye ukazyvayut na to, chto takova sud'ba mnogih kompaktnyh ob'ektov etogo tipa), to my poka i ne dolzhny videt' fenomeny, svyazannye s pul'sarnoi aktivnost'yu.

Mnogim budet interesno pochitat' o mnozhestve oshibochnyh zayavlenii ob obnaruzhenii pul'sara, osobenno vskore posle vzryva (razumeetsya, sleduet govorit' ne o vremeni vzryva, a o vremeni ego registracii na Zemle).


arxiv:0708.2505 Detali radioizlucheniya v pul'sare v Krabe (Radio Emission Signatures in the Crab Pulsar)
Authors: T. H. Hankins, J. A. Eilek
Comments: 26 pages, 10 figures, to appear in ApJ

Nablyudeniya pul'sara v Krabe s vysokim vremennym razresheniem pokazali, chto osnovnoi impul's po svoim svoistvam principial'no otlichaetsya ot interimpul'sa (avtory regulyarno upotryablyayut slovo astonished, chtoby oharakterizovat' svoe vpechatlenie ot obnaruzhennyh otlichii). Po vsei vidimosti za osnovnoi impul's i interpul'sy otvetstvenny raznye mehanizmy izlucheniya (a vo vseh osnovnyh modelyah do sih por polagali, chto mehanizm odin, i razlichie ob'yasnyaetsya geometriei).

Na moi vzglyad eto dolzhno horosho uvyazyvat'sya s nedavnimi rezul'tatami rossiiskih uchenyh (na kotorye avtory rassmatrivaemoi stat'i pochemu-to ne soslalis').


Krab otbivaet nanodrob'


arxiv:0708.2876 Volny Tkachenko kak istochnik kvaziperiodicheskih variacii vrasheniya pul'sara (Tkachenko modes as sources of quasiperiodic pulsar spin variations)
Authors: Jorge Noronha, Armen Sedrakian
Comments: 5 pages, 3 figures, uses RevTex

V neitronnyh zvezdah veshestvo mozhet nahodit'sya v sverhtekuchem sostoyanii. Pri vrashenii sverhtekuchaya zhidkost' razbivaetsya na vihri. V 1966 g. Tkachenko pokazal, chto po sisteme takih vihrei mozhet "gulyat' volna": vihri budut to blizhe drug k drugu, to - dal'she. V 1970 g. Ruderman poproboval prilozhit' etu ideyu v pul'saram: ved' volny Tkachenko dolzhny menyat' moment inercii neitronnoi zvezdy, t.e. vyzyvat' izmenenie perioda vrasheniya. Togda dumali, chto u pul'sara v Krabe nablyudayutsya kolebaniya perioda na vremenah poryadka neskol'kih mesyacev. Ih-to i hotel ob'yasnit' Ruderman. Kak okazalos', u Kraba nikakih kolebanii net - i pro ideyu pochti zabyli.

I vot k idee snova vozvrashayutsya! Avtory probuyut kolichestvenno ob'yasnit' periodicheskuyu modulyaciyu vrasheniya pul'sara 1828-11 za schet voln Tkachenko. Vrode by vse shoditsya.

Mne lichno eta rabota interesno v svyazi s vozmozhnost'yu ob'yasnit' precessiyu istochnika RX J0720.4-3125. Period vrasheniya neitronnoi zvezdy i period kolebanii, svyazannyh s volnami Tkachenko, zhestko privyazany drug k drugu. Period zapodozrennoi precessii v istochnike RX J0720.4-3125 sovpadaet s ozhidaemym periodom voln Tkachenko. Mehanizm voniknoveniya precessii mozhet byt' takim. Glitch (a on, po vsei vidimosti nablyudalsya u RX J0720.4-3125) generiruet volny Tkachenko. Zatem, esli chastota voln Tkachenko i vozmozhnaya chastota precessii neitronnoi zvezdy, opredelyaemaya ee szhatiem, sovpadayut, energiya voln Tkachenko mozhet perekachivat'sya v precessionnoe dvizhenie. Redkost' svobodnoi precessii u neitronnyh zvezd ob'yasnyaetsya tem, chto redko chastota voln Tkachenko sovpadaet s chastotoi precessii. opredelyaemoi szhatiem zvezdy. Pravda, sverhtekuchest' v neitronnyh zvezdah mozhet podavlyat' dolgoperiodicheskuyu precessiyu, no vcherashnyaya stat'ya Giampedakis et al. pokazyvaet, chto dlya dolgoperiodicheskih pul'sarov problemy net.

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


Vypusk 165. 01-13 avgusta 2007

arxiv:0708.0002 1E 1547.0-5408: izluchayushii v radio magnitar s periodom vrasheniya 2 sekundy (1E 1547.0-5408: a radio-emitting magnetar with a rotation period of 2 seconds)
Authors: F. Camilo et al.
Comments: 4 pages, Accepted for publication in ApJ Letters

Navstrechu 40-letiyu otkrytiya radiopul'sarov

Otkryt ochen' interesnyi istochnik.

Sperva on byl obnaruzhen v rentgenovskom diapazone. Togda zhe zapodozrili, chto eto mozhet byt' magnitar (istochnik nahoditsya v ostatke sverhnovoi). Potom udalos' uvidet' radioizluchenie i ustanovit' period - dve sekundy. Zatem byla izmerena pervaya proizvodnaya perioda (vrashenie neitronnoi zvezdy zamedlyaetsya, t.k. ona sil'no zamagnichena). Po zamedleniyu vrasheniya mozhno ocenit' pole - ono okazalos' ravnym 2 1014 Gauss.

Poskol'ku na staryh izobrazheniyah (v rentgene) istochnik ne byl obnaruzhen, to pohozhe, chto eto vtoroi tranzientnyi magnitar (posle XTE J1810-197).


obzor arxiv:0708.1050 Pul'sary: Progress, problemy i perspektivy (Pulsars: Progress, Problems and Prospects)
Authors: Jonathan Arons
Comments: 55 pages, 21 figures. To appear in Springer Lecture Notes on "Neutron Stars and Pulsars, 40 years after the discovery", ed. W.Becker, 2008

Bol'shoi obzor po radiopul'saram.

V poslednee vremya est' sushestvennyi progress i v nablyudeniyah, i v teorii. Tak chto est' chto obsudit'. K sozhaleniyu, ne vse popalo v obzor. Tem ne menee, rekomenduyu.


arxiv:0708.1149 Obnaruzhenie pul'sacii i vozmozhnoi spektral'noi detali v rentgenovskom izluchenii vrashayushegosya radiotranzienta (RRAT) J1819-1458 (Discovery of Pulsations and a Possible Spectral Feature in the X-ray Emission from Rotating Radio Transient J1819-1458)
Authors: M. A. McLaughlin et al.
Comments: 10 pages, 5 figures, accepted by ApJ

Vse pomnyat, chto paru let nazad byl obnaruzhen novyi klass neitronnyh zvezd - vrashayushiesya radiotranzienty (RRATs). Sluchaino, odin iz nih udalos' uvidet' v rentgene - on prosto popal v pole zreniya Chandry. Teper' na osnove glubokih nablyudenii na XMM-Newton avtory rasskazyvayut o dvuh novyh otkrytiyah.

Vo-pervyh, udalos' uvidet' period pul'sacii i v rentgene. On okazalsya ravnym 4.26 sekundy, chto soglasuetsya s dannymi radionablyudenii. Vo-vtoryh, v spektre obnaruzhena spektral'naya detal', kotoruyu mozhno interpretirovat' kak protonnuyu ciklotronnuyu liniyu. Togda rech' idet o magnitnom pole okolo 1014 Gauss. Eto rodnit istochnik s Velikolepnoi semerkoi. Pravda, u poslednih ne nablyudayutsya vspyshki tipa teh, chto vidyat u RRATs.

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


Vypusk 164. 20-31 iyulya 2007

arxiv:0707.2802 Opredelenie mass neitronnyh zvezd v SMC X-1, LMC X-4 i Cen X-3 po dannym VLT/UVES (Determination of the mass of the neutron star in SMC X-1, LMC X-4 and Cen X-3 with VLT/UVES)
Authors: A. van der Meer, L. Kaper, M. H. van Kerkwijk, M. H. M. Heemskerk, E.P.J. van den Heuvel
Comments: 20 pages, Accepted for publication in Astronomy and Astrophysics

Utochneny znacheniya mass neitronnyh zvezd v treh rentgenovskih dvoinyh. Znacheniya takie 1.06+0.11/-0.10 mass Solnca dlya SMC X-1, 1.25+0.11/-0.10 - dlya LMC X-4, i 1.34+0.16/-0.14 - dlya Cen X-3, Obratite vnimanie na nizkoe znachenie dlya SMC X-1.


arxiv:0707.3363 Ochen' glubokie rentgenovskie nablyudeniya anomal'nogo pul'sara 4U 0142+614 (Very deep X-ray observations of the Anomalous X-ray Pulsar 4U 0142+614)
Authors: N. Rea et al.
Comments: 9 pages, 5 figures; accepted for publication on MNRAS

Predstavleny rezul'taty ochen' glubokih nablyudenii odnogo iz anomal'nyh rentgenovskih pul'sarov na XMM-Newton. Nikakih spektral'nyh linii ne obnaruzheno.


arxiv:0707.4067 Uravnenie sostoyaniya plotnogo veshestva: ot yadernyh stolknovenii k neitronnym zvezdam (The Equation of State of Dense Matter : from Nuclear Collisions to Neutron Stars)
Authors: Fiorella Burgio
Comments: 8 pages, 5 figures, invited talk given at NPA3, Dresden, March 2007

Predstavlen ocherednoi raschet uravneniya sostoyaniya vnutri kompaktnyh ob'ektov. Poluchennoe znachenie maksimal'noi massy neitronnoi zvezdy - 1.7 massy Solnca - po vsei vidimosti slishkom malo, choby udovletvorit' nablyudeniyam. Avtor obsuzhdaet, kakim dolzhno byt' povedenie veshestva pri vysokih plotnostyah, chtoby vse bylo OK.


Vypusk 163. 01-19 iyulya 2007

arxiv:0707.0516 Glubokie nablyudeniya slabyh rentgenovskih odinochnyh neitronnyh zvezd na VLT (Deep VLT infrared observations of X-ray Dim Isolated Neutron Stars)
Authors: G. Lo Curto, R.P. Mignani, R. Perna, G.L. Israel
Comments: 6 pages, 2 figures, accepted by A&A on 26-06-2007

Predstavleny rezul'taty glubokih nablyudenii pyati ob'ektov Velikolepnoi semerki v Ik diapazone na VLT. Polucheny tol'ko verhnie predely (primerno 22 velichina v fil'tre H). Po mneniyu avtorov, predely poka nedostatochno gluboki, chtoby sovsem zakryt' model', v kotoroi zametnuyu rol' igrayut ostatochnye diski vokrug neitronnyh zvezd.


arxiv:0707.0937 Nablyudeniya na VLT central'nogo kompaktnogo istochnika v ostatke sverhnovoi Vela Dzhunior (VLT observations of the Central Compact Object in the Vela Jr. supernova remnant)
Authors: R. P. Mignani et al.
Comments: 8 pages, 4 figures, A&Aaccepted

Vela Dzhunior - eto ostatok sverhnovoi v sozvezdii Parusov (vela). "Dzhunior" - chtoby otlichat' ot davno izvestnogo pul'sara (i ostatka) v Vele. Rasstoyanie do ostatka okolo 1 kpk. V nem obnaruzhen central'nyi kompaktnyi rentgenovskii istochnik (CCO). Avtory proveli glubokie nablyudeniya v optike i blizhnem IK na VLT. V optike ob'ekt ne byl obnaruzhen, zato v IK udalos' chto-to rassmotret'. Esli eto ob'ekt, svyazannyi s rentgenovskim istochnikom (a eto poka ne dokazano), to eto mozhet byt' ostatochnyi disk vokrug neitronnoi zvezdy ili zhe sama zvezda. V poslednem sluchae est' mnogo voprosov....


arxiv:0707.1547 Drugaya Geminga: poisk radio i rentgenovskih pul'sacii ot neitronnoi zvezdy, associiruemoi s 3EG J1835+5918 (The Next Geminga: Search for Radio and X-ray Pulsations from the Neutron Star Identified with 3EG J1835+5918)
Authors: J.P. Halpern, F. Camilo, E.V. Gotthelf
Comments: 4 pages, 1 figure, to appear in The Astrophysical Journal

Geminga - izvestnaya neitronnaya zvezda, obnaruzhennaya pervonachal'no po ee gamma-izlucheniyu. Zatem bylo obnaruzheno rentgenovskoe izluchenie, a pozzhe i pul'sacii: kak v rentgene, tak i v radio. 3EG J1835+5918 - eto istochnik, pohozhii na Gemingu. Oboznachenie ukazyvaet, chto sperva s pomosh'yu pribora EGRET byl obnaruzhen gamma-istochnik. Pozzhe bylo obnaruzheno rentgenovskoe izluchenie. A vot pul'sacii vse net i net.

Ne obnaruzheny pul'sacii i po novym dannym, hotya avtory ispol'zovali samuyu moshnuyu artilleriyu, radioteleskop v Grin Benk i rentgenovskuyu observatoriyu Chandra.


arxiv:0707.2100 Relyativistskie dzhety i dlinnye gamma-vspleski ot rozhdayushihsya magnitarov (Relativistic Jets and Long-Duration Gamma-ray Bursts from the Birth of Magnetars)
Authors: N. Bucciantini et al.
Comments: 5 pages, 3 figures, submitted to MNRAS letter, presented at the conference "Astrophysics of Compact Objects", 1-7 July, Huangshan, China

Predstavleny rezul'taty chislennogo modelirovaniya. V rezul'tate kollapsa obrazuetsya sil'no zamagnichenaaya bystrovrashayushayasya neitronnaya zvezda - magnitar. Formiruyutsya dzhety. Parametry obrazovavshegosya ob'ekta pozvolyayut po mneniyu avtorov, govorit' o poyavlenii dlinnogo gamma-vspleska.

Sm. takzhe arXiv:0707.2219 o svyazi sverhnovyh i gamma-vspleskov, a takzhe o vozmozhnosti togo, chto v serdce central'noi mashiny vspleska sidit neitronnaya zvezda, a ne chernaya dyra. I arXiv:0707.2187 o svyazi gamma-vspleskov so zvezdami maloi metallichnosti.


Vypusk 162. 20-30 iyunya 2007

arxiv:0706.3041 Populyacionnyi sintez radio- i gamma- millisekundnyh pul'sarov v galakticheskom diske (Population synthesis of radio and gamma-ray millisecond pulsars from the Galactic disk)
Authors: Sarah A. Story, Peter L. Gonthier, Alice K. Harding
Comments: 38 pages, 10 figures, accepted in ApJ

Sputnik AGILE uzhe na orbite. GLAST dolzhen poletet' v konce goda. Vse eto gamma-observatorii (tol'ko AGILE- malen'kaya, a GLAST - bol'shaya). Vse pomnyat, chto radiopul'sary i drugie neitronnye zvezdy yavlyayutsya (ili mogut yavlyat'sya) gamma-istochnikami. Eto yavlyaetsya motivirovkoi dlya detal'nogo izucheniya etih ob'ektov metodom populyacionnogo sinteza.

Avtory sushestvenno prodivinuli svoyu chislennuyu model'. Osnovnye rezul'taty takovy.
1. V kataloge EGRET est' dostatochnoe kolichestvo neotozhdestvlennyh istochnikov, chast' iz nih, polagayut avtory - eto millisekundnye pul'sary. V dannyh EGRET dolzhno byt' okolo desyatka millisekundnyh radiopul'sarov, a eshe vdobavok okolo dvuh desyatkov millisekundnyh pul'sarov, kotorye ne vidny nam v radio.
2. GLAST konechno zhe uvidit bol'she millisekundnyh pul'sarov. Avtory nazyvayut chislo poryadka 140-150. Podavlyayushee bol'shinstvo iz nih (bolee sotni) - radionevidimye dlya nas.


arxiv:0706.3179 Ostatki sverhnovyh s magnitarami: klyuch k obrazovaniyu magnitarov (Supernova remnants with magnetars: clues to magnetar formation)
Authors: Jacco Vink
Comments: 9 pages, Accepted by Advances in Space Research (Cospar 2006, Beijing, Session E1.4)

Avtor polagaet, chto dannye po ostatkam sverhnovyh, v kotoryh nablyudayutsya kandidaty v magnitary, svidetel'stvuyut protiv togo, chto eti neitronnye zvezdy rozhdayutsya odnovremenno so sverhsil'nymi polyami i ochen' bystrym vrasheniem. Inache byl by dopolnitel'nyi vbros energii v ostatok, chego, vrode by, ne nablyudaetsya.


arxiv:0706.4156 Glitchi anomal'nyh rentgenovskih pul'sarov (Glitches in Anomalous X-ray Pulsars)
Authors: Rim Dib, Victoria M. Kaspi, Fotis P. Gavriil
Comments: 47 pages, 17 figures, 8 tables, submitted to ApJ

Avtory privodyat rezul'taty dlitel'nogo monitoringa anomal'nyh rentgenovskih pul'sarov RXS J170849.0-400910 i 1E 1841-045 na sputnike RossiXTE. Soobshaetsya ob obnaruzhenii chetyreh novyh glitchei u etih ob'ektov. Odin iz glitchei pochti rekordnyi: chastota skaknula pochti na odnu stotysyachnuyu velichiny - eto ochen' mnogo.


Vypusk 161. 09-19 iyunya 2007

arxiv:0706.1511 Pul'sarnye kiki s uchetom modificirovannogo URKA processa i urovnei Landau dlya elektronov (Pulsar Kicks With Modified URCA and Electrons in Landau Levels)
Authors: Ernest M. Henley et al.
Comments: 10 pages, 6 figures

Rassmatrivaetsya ocherednoi variant mehanizma razgona neitronnyh zvezd. V dannom scenarii razgon dlitsya okolo 10 sekund i svyazan s asimmetrichnym izlucheniem neitrino na stadii protoneitronnoi zvezdy. Moment razgona sootvetstvuet vremeni, kogda neitrinosfera tol'ko-tol'ko "vylezla" iz pod poverhnosti neitronnoi zvezdy. Skorost' dolzhna byt' napravlena po magnitnomu polyu (mne eto ne ochen' ponyatno, uchityvaya, chto razgon deistvuet 10 sekund - t.e. mnogo bol'she, chem period vrasheniya zvezdy vokrug svoei osi). Takzhe avtory predskazyvayut lineinuyu korrelyaciyu mezhdu radiosvetimost'yu pul'sara i ego skorost'yu. Voobshe govorya, takogo ne nablyudaetsya.


miniobzor arxiv:0706.1542 Pul'sarnaya fizika i GLAST (Pulsar Physics and GLAST)
Authors: Alice K. Harding
Comments: 5 pages, 2 figures, to appear in Proc. of First GLAST Symposium (Stanford, Feb. 5-8, 2007), eds. S.Ritz, P.F. Michelson, and C.Meegan, AIP Conf. Proc

V konce goda dolzhen byt' zapushen gamma-sputnik GLAST. Odnimi iz osnovnyh ob'ektov dlya nablyudenii na nem budut pul'sary. V korotkoi zametke daetsya obzor, posvyashennyi gamma-izlucheniyu pul'sarov i perspektivam ih nablyudeniya na GLAST'e. Mozhno ozhidat', chto budet vnesena kakaya-to yasnost' vo mnogie aspekty fiziki pul'sarnyh magnitosfer.


Vypusk 160. 01-08 iyunya 2007

arxiv:0706.1054 Kompaktnyi rentgenovskii istochnik 1E 1547.0-5408 v radioobolochke G327.24-0.13: novyi vozmozhnyi primer associacii mezhdu kandidatom v magnitary i kandidatom v ostatki sverhnovyh (The Compact X-ray Source 1E 1547.0-5408 and the Radio Shell G327.24-0.13: A New Proposed Association between a Candidate Magnetar and a Candidate Supernova Remnant)
Authors: Joseph D. Gelfand, B. M. Gaensler
Comments: 11 pages, 5 figures, ApJ accepted

Avtory predstavlyayut rezul'taty nablyudenii v raznyh diapazonah istochnika 1E 1547.0-5408. Po mneniyu avtorov, my imeem delo s magnitarom, k tomu zhe, vo vsei vidimosti, nahodyashimsya v ostatke sverhnovoi. Tak eto ili net na samom dele pokazhut dal'neishie issledovaniya.


Vypusk 159. 22-31 maya 2007

arxiv:0705.3713 Magnitarnaya priroda i mehanizm vspyshki tranzientnogo anomal'nogo pul'sara (The Magnetar Nature and the Outburst Mechanism of a Transient Anomalous X-ray Pulsar)
Authors: Tolga Guver, Feryal Ozel, Ersin Gogus, Chryssa Kouveliotou
Comments: 9 pages, Submitted to ApJ Letters

Seichas schitaetsya standartnym nazyvat' istochniki myagkih povtoryayushihsya gamma-vspleskov (MPG) i anomal'nye rentgenovskie pul'sary (ARP) kandidatami v magnitary. Delo v tom, chto izmerit' pole napryamuyu ochen' neprosto. Poka eto bylo sdelano lish' dlya odnogo MPG vo vremya vspyshki, da i to nekotorye skeptiki podvergayut interpretaciyu etih nablyudenii somneniyu. S pomosh'yu dostatochno pryamyh nablyudenii avtory etoi stat'i podtverzhdayut magnitarnuyu prirodu odnogo iz ARP (hotya, opredelennye model'nye predpolozheniya avtoram vse-taki prishlos' sdelat'). Rech' idet o tranzientnom ARP J1810-197.

Pole poluchaetsya ravnym primerno 3 1014 Gauss. Eto neploho soglasuetsya s dannymi po zamedleniyu vrasheniya dannoi neitronnoi zvezdy.

Peremennost' spektra (ot radio do rentgena) ARP J1810-197 obsuzhdaetsya v stat'e arxiv:0705.4095. Opredelenie rasstoyaniya do 1810-197 po dannym radionablyudenii yavlyaetsya temoi raboty arxiv:0705.4403.

Dannye po drugomu ARP predstavleny temi zhe avtorami v rabote arxiv:0705.3982.


arxiv:0705.3717 Akkuratnoe opredelenie koordinat po rentgenovskim dannym i vsevolnovye nablyudeniya neitronnoi zvezdy RBS 1774 (Accurate X-ray position and multiwavelength observations of the isolated neutron star RBS 1774)
Authors: N. Rea et al.
Comments: 8 pages, 9 figures, accepted for publication on MNRAS

Opisany rezul'taty vsevolnovyh nablyudenii odnoi iz neitronnyh zvezd, vhodyashih v t.n. Velikolepnuyu semerku. Esli korotko: nichego, krome teplovogo rentgena, ne vidno. Postavleny ochen' glubokie predely i v optike, i v IK, i, chto vazhno, v radio.


Vypusk 158. 12-21 maya 2007

arxiv:0705.1705 O prirode korotkogo gamma-vspleska GRB 050906 (On the nature of the short duration GRB 050906)
Authors: A.J. Levan et al.
Comments: 8 pages, 5 figures, accepted for publication in MNRAS

Esli korotko, to avtory polagayut, chto vsplesk mozhet schitat'sya eshe odnim kandidatov v nipervspyshki vnegalakticheskih magnitarov. Reshayushim argumentom sluzhit nalichie v oblasti lokalizacii vspleska otnositel'no blizkoi galaktiki s moshnym zvezdoobrazovaniem IC 328.


arxiv:0705.1973 Gody monitoringa anomal'nogo rentgenovskogo pul'sara 4U 0142+61 na sputnike RXTE: dolgopreiodicheskaya peremennost' (Years of RXTE Monitoring of Anomalous X-ray Pulsar 4U 0142+61: Long-Term Variability)
Authors: R. Dib, V. M. Kaspi, F. P. Gavriil.
Comments: 28 pages, 8 figures, accepted by ApJ

V moih obzorah davno zameten perekos v storonu moih sobstvennyh interesov v astrofizike. Poetomu ne udivlyaites' bol'shomu kolichestvu ssylok na stat'i po neitronnym zvezdam. Vot ocherednaya.

Avtory predstavlyayut rezul'taty mnogoletnego monitoringa odnogo iz kandidatov v magnitary. S odnoi storony, nikakih superotkrytii net. S drugoi, dannye stavyat interesnye voprosy pered standartnoi magnitarnoi teoriei.


obzor arxiv:0705.2708 Nedra neitronnyh zvezd i uravnenie sostoyaniya sverhplotnogo veshestva (Neutron Star Interiors and the Equation of State of Superdense Matter)
Authors: F. Weber et al.
Comments: 33 pages, 20 figures; Invited review talk presented at "Neutron Stars and Pulsars: About 40 years after the discovery," Physics Center Bad Honnef, Germany, 14-19 May 2006. To be published in Springer Lecture Notes

Ocherednoi bol'shoi obzor po vnutrennemu sostoyaniyu neitronnyh zvezd. Osoboe vnimanie avtory udelyayut ekzoticheskim fazam (kvarkam, giperonam i tp.).


arxiv:0705.2713 Unikal'naya sverhnovaya 2005bf tipa Ib v nebulyarnoi faze: vozmozhnoe rozhdenie sil'no zamagnichennoi neitronnoi zvezdy (The Unique Type Ib Supernova 2005bf at Nebular Phases: A Possible Birth Event of A Strongly Magnetized Neutron Star)
Authors: K. Maeda et al.
Comments: 16 pages, 12 figures. Accepted by the Astrophysical Journal

Opisany dannye po neobychnoi sverhnovoi tipa Ib. Avtory predlagayut interpretaciyu, soglasno kotoroi imeet mesto dopolnitel'naya zakachka energii blagodarya rabote molodogo magnitara - bystro vrashayusheisya neitronnoi zvezdy s sil'nym magnitnym polem.


Vypusk 157. 01-11 maya 2007

arxiv:0705.0978 Rentgenovskii taiming PSR J1852+0040 v Kesteven 79: ukazanie na neitronnuyu zvezdu, slabozamagnichennuyu pri rozhdenii (X-ray Timing of PSR J1852+0040 in Kesteven 79: Evidence of Neutron Stars Weakly Magnetized at Birth)
Authors: J. P. Halpern, E. V. Gotthelf, F. Camilo, F. D. Seward
Comments: 8 pages, 3 figures, to appear in The Astrophysical Journal

Nedavno eti zhe avtory pisali o tom, chto istochnik 1E 1207.4-5209 v ostatke sverhnovoi PKS 1209-51/52 yavlyaetsya primerom neitronnoi zvezdy, rodivsheisya s otnositel'no dlinnym periodom vrasheniya i slabym magnitnym polem. V dannoi zhe stat'e detal'no obsuzhdaetsya drugoi primer.

Avtory prodolzhayut razvivat' gipotezu o tom, chto slabye nachal'nye magnitnye polya svyazany s dlinnymi nachal'nymi periodami (v etoi modeli pole generiruetsya s pomosh'yu dinamo-mehanizma, chto trebuet bystrogo vrasheniya). Krome togo, po mneniyu avtorov, sushestvennaya akkreciya na slabozamagnichennye molodye neitronnye zvezdy.


arxiv:0705.1011 Otkrytie odinochnogo kompaktnogo ob'ekta na bol'shoi galakticheskoi shirote (Discovery of an Isolated Compact Object at High Galactic Latitude)
Authors: R. E. Rutledge, D. B. Fox, A. H. Shevchuk
Comments: 19 pages, 4 figures, ApJ, submitted

Po vsei vidimosti otkryt interesnyi kompaktnyi ob'ekt, veroyatnee vsego - neitronnaya zvezda. Otkrytie bylo sdelaono po arhivnym dannym sputnika ROSAT. Istochnik demonstriruet teplovoe izluchenie, no nahoditsya slishkom vysoko nad galakticheskoi ploskost'yu. Esli predpolozhit', chto eto ob'ekt tipa Velikolepnoi semerki, to chtoby popast' na takuyu vysotu, emu nuzhno bylo by letet' so skorost'yu okolo 7000 km/s. Poetomu avtory polagayut, chto eto mozhet byt' ob'ekt tipa millisekundnyh pul'sarov. No i tut est' nemalo slozhnostei.

Na moi vzglyad (i avtory, razumeetsya, takzhe rassmatrivayut etu gipotezu), my imeem delo s ob'ektom tipa Cas A, tol'ko raz v 10 starshe.


Vypusk 155. 13-23 aprelya 2007

arxiv:0704.2255 Precezionnyi taiming rentgenovskogo pul'sara 1E 1207.4-5209: stabil'naya neitronnaya zvezda, slabo zamagnichennaya pri rozhdenii (Precise Timing of the X-ray Pulsar 1E 1207.4-5209: A Steady Neutron Star Weakly Magnetized at Birth)
Authors: E. V. Gotthelf, J. P. Halpern
Comments: 5 pages, 2 figure, Latex, emulateapj style. Submitted to ApJ Letters

Est' takaya odinochnaya neitronnaya zvezda v ostatke svehnovoi - istochnik 1E 1207.4-5209. Znamenit on tem, chto v ego spektre bylo naideno neskol'ko spektral'nyh linii (uchityvaya te, chto nahodyatsya na predele obnaruzhimosti - chetyre). Prichem, raspredelenie linii po energii obrazuet geometricheskuyu posledovatel'nost', t.e., est' oshushenie, chto eto ciklotronnaya liniya i ee garmoniki. Mozhet byt' eto i ne tak, no dopustim. Togda, mozhno opredelit' magnitnoe pole. Pravda, nado ponyat' protonnaya li eto liniya, ili elektronnaya. Ocenka polya budet razlichat'sya primerno v tysyachu raz (otnoshenie mass elektrona i protona). Esli liniya protonnaya, kak schitali v nachale, to pole budet bol'shoe.

Rezul'taty, predstavlennye v rassmtrivaemoi stat'e, govoryat o tom, chto pole u neitronnoi zvezdy malen'koe. Ustanovleno eto po izmereniyam tempa zamedleniya vrasheniya zvezdy. Esli prinyat' gipotezu i tom, chto zamedlenie mozhno opisat' t.n. magnito-dipol'noi formuloi, to poluchim ocenku polya okolo 10 v 11 Gauss ili men'she. Eto mozhet nahoditsya v soglasii s tem, chto linii taki svyazany s elektronami.

Novye rezul'taty polucheny ne s pomosh'yu novyh nablyudenii. Avtory proveli pereobrabotku uzhe imeyushihsya dannyh. Vidimo, v bolee rannem variante obrabotki byla dopushena netochnost'.

Interesen eshe odin moment. Energovydelenie neitronnoi zvezdy bol'she, chem mozhet dat' zamedlenie vrasheniya. Eto govorit o tom, chto rentgenovskaya svetimsot' v osnovnom dolzhna byt' svyazana s ohlazhdeniem neitronnoi zvezdy ili s akkreciei.

Teper' ves' kompleks dannyh govorit o tom, chto dannaya neitronnaya zvezda rodilas' s periodom okolo 0.4 sek (chto blizko k nablyudaemomu periodu) i malym magnitnym polem, po sravneniyu so standartnymi polyami radiopul'sarov i, tem bolee, magnitarov. Pryamoe otkrytie sochetaniya otnositel'no dlinnyh nachal'nyh periodov vrasheniya i otnositel'no slabogo polya pozvolyaet prodvinut'sya v ponimanii molodyh neitronnyh zvezd, ne proyavlyayushih pul'sarnoi ili magnitarnoi aktivnosti. Vozmozhno, chto pole generiruetsya v novorozhdennoi neitronnoi zvezde, a effektivnost' generacii zavisit ot tempa vrasheniya. S drugoi storony, u molodyh pul'sarov kakoi-to chetkoi zavisimosti takogo tipa ne vyyavleno.

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


arxiv:0704.2415 Nablyudeniya v blizhnem IK i v rentgene zagadochnogo G70.7+1.2 (Near-Infrared and X-ray Observations of the Enigmatic G70.7+1.2)
Authors: P. B. Cameron, S. R. Kulkarni
Comments: 13 pages, 4 figures. Submitted to ApJL, referee's comments incorporated

Priroda poroyu podkidyvaet interesnye zagadki. Nichego superfundamental'nogo v nih net, no mne lichno oin vsegda nravyatsya. Sut' zagadki svoditsya k sleduyushemu: chto zhe my vidim?

G70.7+1.2 - eto tumannost', nablyudaemaya v opticheskom i radio diapazonah. Krome togo, v nei est' yarkaya zvezda, kotoruyu nablyudayut v IK, t.k. veliko pogloshenie. Polagali, chto my imeem delo s dvoinoi sistemoi, sostoyashei iz Be- zvezdy i radiopul'sara.

Avtory stat'i proveli glubokie nablyudeniya v IK (na Keke) i v rentgene (na Chandre). Byl obnaruzhen rentgenovskii istochnik, ne sovpadayushii s Be-zvezdoi. Tot zhe istochnik viden i v blizhnem IK. Novaya interpretaciya takova. V tumannosti est' Be-zvezda i dvoinaya sistema, sostoyashaya iz B-zvezdy i neitronnoi zvezdy, skoree vsego radiopul'sara. Sleduyushaya zadacha - glubokii poisk pul'sara. Esli ne naidut - to zagadka ostanetsya. Interesno!


Vypusk 154. 01-12 aprelya 2007

miniobzor arxiv:0704.1215 Dvoinye neitronnye zvezdy: ukazanie na dva razlichnyh mehanizma obrazovaniya (Double Neutron Stars: Evidence For Two Different Neutron-Star Formation Mechanisms)
Authors: E.P.J. van den Heuvel
Comments: 9 pages. Invited talk at he Multicoloured Landscape of Compact Objects and their Explosive Origins', Cefalu', 2006 June 11-24 (AIP Conf. Proc.), eds. L. Burderi et al., i

Izvestno 9 dvoinyh sistem, sostoyashih iz dvuh neitronnyh zvezd. S nimi svyazana odna zagadka. Slishkom mnogie iz nih imeyut malen'kie ekscentrisitety. Esli uchest', chto soglasno dannym po obychnym radiopul'saram neitronnye zvezdy rozhdayutsya s bol'shimi skorostyami (t.n. kik) poryadka 300-400 km/s, to malye ekscentrisitety predstavlyayutsya zagadochnymi. Po vsei vidimostim, te vzryvy sverhnovyh, kotorye privodyat (v srednem) k poyavleniyu odinochnyh pul'sarov i pul'sarov v massivnyh dvoinyh sistemah, razlichayutsya. Van den Hevel obsuzhdaet vozmozhnye puti resheniya zagadki. Na dannyi moment slozhilsya sleduyushii vzglyad. Vtorichnye komponenty massivnyh dvoinyh sistem ispytyvayut ne obychnyi vzryv sverhnovoi, svyazannyi s kollapsom zheleznogo yadra, a kollaps kislorodno-neonovo-magnievogo yadra. Veroyatnee vsego, eto yavlyaets isklyuchitel'noi osobennost'yu dvoinyh sistem. V odinochnyh zvezdah takie yadra v konce koncov prevrashayutsya v belye karliki.


Vypusk 152. 10-19 marta 2007

obzor astro-ph/0703233 Rozhdenie strannyh zvezd: kinetika, gidrodinamika i fenomenologiya sverhnovyh i gamma-vspleskov (The birth of strange stars: kinetics, hydrodynamics and phenomenology of supernovae and GRBs)
Authors: J.E. Horvath
Comments: 23 pp., 1 .eps figure

Esli kvarkovye zvezdy sushestvuyut, to oni kak-to obrazuyutsya. T.e., est' nekotoryi dlyashiisya vo vremeni process, v kotorom obychnaya neitronnaya zvezda (ili protoneitronnaya zvezda) prevrashaetsya v kvarkovuyu. Process etot neprostoi, i neudivitel'no, chto nikakoi yasnosti v etom voprose net.

V stat'e avtor vo-pervyh, kratko opisyvaet kvarkovye zvezdy, a vo-vtoryh, daet obzor sovremennyh issledovanii, posvyashennyh processu obrazovaniya kvarkovyh zvezd.


astro-ph/0703246 Glubokie poiski radio pul'sacii i vspyshek ot chetyreh yuzhnyh anomal'nyh rentgenovskih pul'sarov (Deep Searches for Radio Pulsations and Bursts from Four Southern Anomalous X-ray Pulsars)
Authors: Fronefield Crawford, Jason W. T. Hessels, Victoria M. Kaspi
Comments: 6 pages, including 1 table. Accepted for publication in ApJ

Predstavleny rezul'taty nablyudenii chetyreh anomal'nyh rentgenovskih pul'sarov na Parksovskom (Parkes) teleskope. Istochniki ne byli zaregistrirovany, t.e. est' tol'ko verhnie predely na ih radioizluchenie. Vo vremya nablyudenii istochniki ne proyavlyali vspyshechnoi aktivnosti v rentgenovskom diapazone. T.o., avtory polagayut, chto rezul'taty mogut sluzhit' podtverzhdeniem togo, chto v spokoinom sostoyanii anomal'nye pul'sary ne izluchayut v radio.


astro-ph/0703267 Dissipaciya magnitnogo polya v kore neitronnyh zvezd: ot magnitarov k odinochnym neitronnym zvezdam (Magnetic field dissipation in neutron star crusts: from magnetars to isolated neutron stars)
Authors: J.A. Pons, U. Geppert
Comments: 14 pages, 10 figures

Avtory rassmatrivayut zatuhanie magnitarnyh magnitnyh polei v kore. Odin iz osnovnyh vyvodov sostoit v tom, chto ob'ekty Velikolepnoi semerki v ramkah takogo scenariya dolzhny yavlyat'sya potomkami magnitarov. Na moi vzglyad, zdes' est' nekotorye trudnosti. Delo v tom, chto temp rozhdeniya o''ektov tipa Velikolepnoi semerki dovol'no vysok. On v neskol'ko raz vyshe, chem temp rozhdeniya anomal'nyh rentgenovskih pul'sarov i istochnikov myagkih povtoryayushihsya gamma-vspleskov (eti istochniki yavlyayutsya kandidatami v magnitary). Protivorechie mozhno razreshit' tol'ko predpolozheniem, chto bOl'shaya chast' molodyh magnitarov ne proyavlyaet aktivnosti (ili periody aktivnosti chrezvychaino korotkie).


astro-ph/0703287 Predely na massu i radius millisekundnogo rentgenovskogo pul'sara SAX J1808.4-3658 (Limits on Mass and Radius for the ms-Period X-ray Pulsar SAX J1808.4-3658)
Authors: Denis A. Leahy, Sharon M. Morsink, Coire Cadeau
Comments: 6 pages, 2 figures. Submitted to ApJ Letters

Avtory dayut ocenku massy i radiusa neitronnoi zvezdy, vhodyashei v dvoinuyu sistemu SAX J1808.4-3658. Sushestvenno, chto ih rezul'taty protivorechat osnovnoi masse drugih. A imenno, dannye govoryat o tom, chto massa i radius sootvetstvuyut t.n. myagkomu uravneniyu sostoyaniya (eto govorit o tom, chto neitronnaya zvezda kak by bolee szhimaema). Uravnenie sostoyaniya dolzhno byt' odno! Maksimum, chto mozhet byt', eto sosushestvovanie neskol'kih faz (naprimer, obychnye adronnye neitronnye zvezdy i kvarkovye zvezdy), t.e. uravnenie sostoyaniya budet sostoyat' iz dvuh chastei, perehodyashih (skachkom) drug v druga na nekotoroi krticheskoi plotnosti. Poka vse dannye svidetel'stvovali v pol'zu zhestkih uravnenii sostoyaniya (naprimer, sushestvovanie massivnyh neitronnyh zvezd, s massami bolee 2 solnechnyh, a takzhe analogichnye privodimym v stat'e dannye po nablyudeniyam rentgenovskih istochnikov).

Skoree vsego okazhetsya, chto ocenki, sdelannye etoi stat'e, soderzhat v sebe kakuyu-to neuchtennuyu neopredelennost'. Tem ne menee, rezul'tat zasluzhivaet vnimaniya.


astro-ph/0703336 VLBA izmereniya transversal'noi skorosti magnitara XTE J1810-197 (VLBA measurement of the transverse velocity of the magnetar XTE J1810-197)
Authors: D. J. Helfand et al.
Comments: Accepted for publication in The Astrophysical Journal. Six pages, 2 figures

Anomal'nyi rentgenovskii pul'sar XTE J1810-197 udalos' pronablyudat' v radiodiapazone. Krome vazhnoi informacii o rabote magnitara, radionablyudeniya dayut vozmozhnost' opredelit' nekotorye vazhnye parametry neitronnoi zvezdy. Naprimer, mozhno izmerit' ee skorost'. Tochnee, mozhno opredelit' proekciyu skorosti na nebesnuyu sferu, skorost' vdol' lucha zreniya ostaetsya neizvestnoi. Poluchennoe znachenie sostavlyaet primerno 200-300 km/s. Eto nemnogo dlya neitronnyh zvezd. T.o., staraya gipoteza o tom, chto magnitary (anomal'nye rentgenovskie pul'sary i istochniki myagkih povtoryayushihsya gamma-vspleskov) pogolovno yavlyayutsya bystro dvizhushimisya ob'ektami, navernoe bolee ne imeet prava na sushestvovanie.


astro-ph/0703343 Rasstoyanie do odinochnoi neitronnoi zvezdy RX J0720.4-3125 (The Distance to the Isolated Neutron Star RX J0720.4-3125)
Authors: D. L. Kaplan, M. H. van Kerkwijk, J. Anderson
Comments: 17 pages, 8 figures. To be published in ApJ

S pomosh'yu opticheskih nablyudenii na Kosmicheskom teleskope udalos' opredelit' parallaks eshe odnoi neitronnoi zvezdy iz Velikolepnoi semerki. Rasstoyani okazalos' ravnym 270-530 pk. Transversal'naya skorost' 140-270 km/c. Po vsei vidimosti, zvezda rodilas' v OV associacii Trumpler okolo milliona let nazad.


astro-ph/0703346 Temp rozhdeniya magnitarov (The birthrate of magnetars)
Authors: R. Gill, J. Heyl
Comments: 7 pages, to be submitted to MNRAS

Avtory rasschityvayut temp rozhdeniya magnitarov i ob'ektov tipa Velikolepnoi semerki. Dlya pervyh poluchaetsya znachenie raz v 500 let, dlya vtoryh - na poryadok bol'she. Chto nazyvaetsya, "ob etom-to davno i govorili bol'sheviki". Ya neodnokratko podcherkival, chto temp rozhdeniya Velikolepnoi semerki slishkom velik, chtoby sdelat' eti ob'ekty "starymi magnitarami".


Vypusk 151. 01-09 marta 2007

obzor astro-ph/0703116 Teoriya pul'sarnogo vetra i tumannostei (The theory of pulsar winds and nebulae)
Authors: J. G. Kirk, Y. Lyubarsky, J. Petri
Comments: 33 pages invited review, 363rd Heraeus Seminar "Neutron Stars and Pulsars", Bad Honnef, 2006

Heraeus Seminar slavitsya svoimi tradiciyami. Osobenno raduyut obzornye stat'i, poyavlyayushiesya v ego sbornikah. Dannaya ne yavlyaetsya isklyucheniem, i tozhe raduet.

Pul'sarnyi veter i tumannosti, "vyduvaemye" pul'sarami, v poslednie gody yavlyaeyutsya ob'ektami pristal'nogo vnimaniya i ozhivlennogo interesa. Svyazano eto s tem, chto novye pribory, v pervuyu ochered' Chandra, dali vozmozhnost' rassmotret' v nih mnozhestvo interesnyh detalei (vse, navernoe, pomnyat rentgenovskie izobrazheniya vnutrennih, okolopul'sarnyh, chastei krayuovidnoi tumannosti s torom i dzhetami). V obzore skrupulezno opisyvayutsya sovremennye idei po opisaniyu processov v pul'sarnom vetre i tumannostyah.


astro-ph/0703181 Pul'siruyushee rentgenovskoe izluchenie ot Pul'sara A v dvoinoi sisteme J0737-3039 (Pulsed X-ray Emission from Pulsar A in the Double Pulsar System J0737-3039)
Authors: S. Chatterjee et al.
Comments: 6 pages, 3 figures, emulateapj; submitted to ApJ

Po dannym nablyudenii na kosmicheskoi rentgenovskoi observatorii Chandra obnaruzheno pul'siruyushee rengenovskoe izluchenie ot millisekundnogo pul'sara v izvestneishei sisteme J0737-3039.

J0737-3039 - eto edinstvennaya sistema, sostoyashaya iz dvuh radiopul'sarov. Rentgenovskoe izluchenie ot etogo istochnika uzhe bylo zaregistrirovano, odnako kakih-libo periodicheskih izmenenii potoka obnaruzheno ne bylo. Novye nablyudeniya pozvolili obnaruzhit' pul'sacii s periodom, ravnym periodu vrasheniya millisekundnogo pul'sara (Pul'sar A). Pul'sacii na chastote vtorogo pul'sara ili modulyaciya za schet orbital'nogo dvizheniya poka (?) ne obnaruzheny.


Vypusk 150. 15-28 fevralya 2007

obzor astro-ph/0702426 Teplovoe izluchenie odinochnyh neitronnyh zvezd: teoreticheskie i nablyudatel'nye aspekty (Thermal emission from isolated neutron stars: theoretical and observational aspects)
Authors: Vyacheslav E. Zavlin
Comments: Review lecture given at the 363-rd Heraeus Seminar on Neutron Stars and Pulsars held on May 14-19, 2006 in Bad Honnef (Germany); to be published as a Springer Lecture Notes; 37 pages, 14 figures;

Podrobnyi obzor po ochen' aktual'noi seichas teme. Delo v tom, chto teplovoe izluchenie neitronnyh zvezd opredelyaetsya processami v ih nedrah. T.o., nablyudeniya etogo izlucheniya pozvolyayut nam kosvenno zaglyanut' v nedra neitronnyh zvezd i popytat'sya chto-to uznat' o fizicheskih processah, prohodyashih pri ekstremal'nyh usloviyah. Krome togo, neitronnye zvezdy obladayut ochen' interesnymi atmosferami. S nimi eshe mnogoe neponyatno, a na spektry teplovogo izlucheniya oni vliyayut kriticheskim obrazom.


obzor astro-ph/0702698 Lyubopytnye svoistva raskruchennyh pul'sarov i vozmozhnost' vysokotochnogo taiminga (Curious properties of the recycled pulsars and the potential of high precision timing)
Authors: Matthew Bailes
Comments: 15 pages, 8 figures, To appear in proceedings of "A life with stars", a conference held in honour of Ed van den Heuvel, Amsterdam, Aug 2005), New Ast. Rev. accepted Feb 2007

Daetsya obzor svoistv raskruchennyh pul'sarov. Vrashenie etih ob'ektov bylo uskoreno za schet akkrecii v tesnoi dvoinoi sisteme. Avtor privodit neskol'ko poleznyh grafikov, a takzhe obsuzhdaet svyaz' nekotoryh parametrov raskruchennyh pul'sarov s massoi ih kompan'onov.


Vypusk 149. 01-14 fevralya 2007

miniobzor astro-ph/0702188 INTEGRAL i magnitary (INTEGRAL and Magnetars)
Authors: D. Gotz, et al.
Comments: 8 pages, 9 figures, Proceedings of the 6th INTEGRAL Workshop, Moscow, 2006 07 03-07, ESA SP-622

Sputnik INTEGRAL vnes sushestvennyi vklad i issledovaniya magnitarov - istochnikov myagkih povtoryayushihsya gamma-vspleskov (MPG) i anomal'nyh rentgenovskih pul'sarov (ARP). V pervuyu ochered', sleduet otmetit' otkrytie "zhestkih hvostov" v spektrah ARP. Takzhe, INTEGRAL zaregistriroval mnozhestvo vspleskov MPG. Nu i, razumeetsya, pronablyudal gigantskuyu vspyshku dekabrya 2004 goda.

V stat'e summirovany vse osnovnye rezul'taty, hotya osnovnoe vnimanie udeleno rezul'tatam, poluchennym samim avtorami.


obzor astro-ph/0702235 Struktura i ostyvanie neitronnyh zvezd (Structure and cooling of compact stars)
Authors: Hovik Grigorian
Comments: 22 pages, 9 figures, Lecture notes for the Helmholtz International Summer School on "Dense Matter in Heavy-Ion Collisions and Astrophysics", JINR, Dubna, August 21 - September 1, 2006

Ponyatnyi obzor, posvyashennyi vnutrennemu stroeniyu i teplovoi evolyucii neitronnyh zvezd.


gr-qc/0702039 Verhnie predely na gravitacionno-volnovoe izluchenie dlya 78 pul'sarov (Upper limits on gravitational wave emission from 78 radio pulsars)
Authors: The LIGO Scientific Collaboration: B. Abbott, et al, M. Kramer, A. G. Lyne
Comments: 21 pages

LIGO prodolzhaet sbor dannyh. Komanda regulyarno vydaet verhnie predely na gravitacionno-volnovoe izluchenie ot radiopul'sarov (obo vsem etom, kstati, mozhno pochitat' vo vtorom nomere "Vokrug Sveta"). Rastet chislo issledovannyh pul'sarov, i predely stanovyatsya vse luchshe i luchshe. Samyi zhestkii na segodnyashnii den' daet parametr ekvatorial'noi elliptichnosti uzhe na urovne 10-6 (ob opredelenii etogo parametra sm., naprimer, gr-qc/0508096, str. 2 uravnenie 2). Eto uzhe na urovne ozhidaemogo. T.e., po vsei vidimosti, nedalek tot den', kogda poyavitsya i signal. LIGO ili VIRGO pervym ego poimayut - uvidim.


obzor astro-ph/0702254 O nastoyashem i budushem pul'sarnoi astronomii (On the Present and Future of Pulsar Astronomy)
Authors: W.Becker et al.
Comments: 30 pages, Summary of the Joined Discussion (JD02) held at the XXVI IAU General Assembly in 2006 August in Prague. To appear in "Highlights of Astronomy, Volume 14", ed. K.A. van der Hucht

Dan obzor dokladov, predstavlennyh na poslednei General'noi assamlee MAS v Prage. Stat'ya daet neplohoi predstavlenie o tom, chto seichas proishodit v oblasti izucheniya pul'sarov.


astro-ph/0702336 Poisk s pomosh'yu H.E.S.S. pul'siruyushego gamma-izlucheniya ochen' vysokoi energii ot molodyh radiopul'sarov (Search for Pulsed VHE Gamma-Ray Emission from Young Pulsars with H.E.S.S)
Authors: The HESS Collaboration: F.Aharonian, et al
Comments: 13 pages, 11 figures, accepted for publication in A&A

H.E.S.S. otnablyudal desyatok pul'sarov, ot kotoryh mozhno bylo by ozhidat' zametnogo potoka gamma-izlucheniya vysokoi energii. Rezul'tat nulevoi. Uchityvaya velikolepnye parametry H.E.S.S., eto ochen' ser'eznye verhnie predely. Oni ukazyvayut na to, chto na energiyah poryadka TeV v spektre pul'sarov dolzhen byt' zagib. Eto daet ser'eznye ogranicheniya na modeli izlucheniya pul'sarov.


astro-ph/0702347 Neobychnyi dvoinoi pul'sar PSR J1744-3922: peremennost' radio potoka, nablyudeniya v blizhnem IK i evolyuciya (The Unusual Binary Pulsar PSR J1744-3922: Radio Flux Variability, Near-infrared Observation and Evolution)
Authors: R. P. Breton et al.
Comments: 18 pages, 8 figures, accepted for publication of ApJ

Avtory polagayut, chto etot neobychnyi pul'sar i eshe neskol'ko drugih obrazuyut osobyi klass ob'ektov, vydelyayushiisya sredi osnovnoi massy dvoinyh pul'sarov. V chastnosti, dlya ih formirovaniya nuzhen osobyi evolyucionnyi kanal.

Magnitnoe pole pul'sara okazyvaetsya slishkom sil'nym, a period slishkom dlinnym, uchityvaya parametry dvoinoi sistemy. Krome togo, pul'sar pokazyvaet sil'nuyu peremennost', chto netipichno dlya dvoinyh pul'sarov s malomassivnymi kompan'onami na orbitah s korotkim orbital'nym periodom.


Vypusk 146. 01-21 dekabrya 2006

obzor astro-ph/0612144 Obrazovanie dvoinyh kompaktnyh ob'ektov (Formation of Double Compact Objects)
Authors: V. Kalogera et al.
Comments: 55 pages, 16 figures, to appear in the Bethe Centennial Volume of Physics Reports, eds. G. E. Brown, V. Kalogera, E.P.J. van den Heuvel

Bol'shoi obzor, posvyashennyi v osnovnom, obrazovaniyu dvoinyh neitronnyh zvezd. Odnako, krome nih, rassmatrivayutsya i sistemy s chernymi dyrami i belymi karlikami. Avtory chestno pishut, chto dayut svodku v osnovnom svoih rezul'tatov, tak chto o rabotah drugih grupp pishut dovol'no-taki mimohodom.

Napomnyu, chto vsya eta deyatel'nost' po povodu dvoinyh kompaktnyh ob'ektov vazhna, v pervuyu ochered', v svyazi s rabotoi detektorov gravitacionnyh voln. Takzhe, dvoinye kompaktyne ob'ekty interesny kak vozmozhnye istochniki korotkih gamma-vspleskov. Nu i prosto, dvoinye radiopul'sary - luchshaya laboratoriya po proverke mnogih interesnyh effektov, vklyuchaya OTO. Krome togo, ne nado zabyvat', chto obnaruzhenie sistemy pul'sar plyus chernaya dyra ne za gorami, i obnaruzhenie takogo "zverya" gotovit nam mnogo otkrytii chudnyh.


astro-ph/0612289 Gigantskaya vspyshka SGR 1806-20 i ee komptonovskoe otrazhenie ot Luny (Giant Flare in SGR 1806-20 and Its Compton Reflection from the Moon)
Authors: D.D.Frederiks et al.
Comments: 29 pages including 18 figures; to appear in Astronomy Letters, 2007, 33, p 1-18

Nakonec-to poyavilas' polnaya i okonchatel'naya versiya stat'i ob obnaruzhenii otrazhennogo signala gipervspyshki SGR 1806-20 v dekabre 2004 goda!

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


obzor astro-ph/0612440 Nablyudeniya neitronnyh zvezd: prognoz dlya ravneniya sostoyaniya (Neutron Star Observations: Prognosis for Equation of State Constraints)
Authors: James M. Lattimer, Maddapa Prakash
Comments: 70 pages, 19 figures, submitted to Hans Bethe Centennial Physics Reports

Ocherednoi bol'shoi obzor iz sbornika, posvyashennogo Gansu Bete. Na etot raz temoi yavlyayutsya neitronnye zvezdy. Avtory v detalyah obsuzhdayut, kak poslednie dannye nablyudenii pomogayut ogranichit' teorii, opisyvayushie vnutrennee stroenie neitronnyh zvezd. Ved' astrofizicheskie dannye po etim ob'ektam yavlyayutsya unikal'nymi v smysle izucheniya povedeniya holodnogo veshestva pri sverhyadernyh plotnostyah.


astro-ph/0612501 Otkrytie 7-misekundnyh pul'sacii ot odinochnoi neitronnoi zvezdy RX J1856.5-3754 po nablyudeniyam na XMM-Newton (XMM-Newton discovery of 7 s pulsations in the isolated neutron star RX J1856.5-3754)
Authors: Andrea Tiengo, Sandro Mereghetti
Comments: Submitted to The Astrophysical Journal Letters

Esli eto pravda, to eto ochen' vazhno dlya astrofiziki neitronnyh zvezd. Obnaruzhen period u samogo pervogo iz ob'ektov Velikolepnoi semerki. Do etogo nikomu ne udavalos' uvidet' pul'sacii, ibo ih uroven' ochen' nevysok. No vot na HMM-N'yutone, s ego kolossal'noi sobirayushei poverhnost'yu, na urovne 1.5 procenta udalos' uvidet' pul'sacii.

Period sostavlyaet 7 sekund. T.o., teper' vse sem' "kovboev" imeyut izmerennye periody.

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


Vypusk 145. 11-30 noyabrya 2006

astro-ph/0611318 Gigantskaya vspyshka 27 dekabrya istochnika SGR 1806-20 (The Giant Flare of December 27, 2004 from SGR 1806-20)
Authors: Steven E. Boggs et al.
Comments: 32 pages, 14 figures, submitted to ApJ

Pochti dva goda nazad proizoshla gigantskaya vspyshka magnitara SGR 1806-20, a stat'i vse poyavlyayutsya i poyavlyayutsya.... V dannoi predstavlen detal'nyi analiz na osnove dannyh indiiskogo sputnika RHESSI. Krome gamma-detektorov, kotorye "oslepli" v moment maksimuma vspyshki, na ego bortu byli i detektory chastic, kotorye vse-taki pozvolyayut poluchit' dannye o vspleske dazhe vo vremya naibol'shego potoka.


obzor astro-ph/0611398 Dvoinye i raskruchennye pul'sary: 30 let posle otkrytiya (Binary and recycled pulsars: 30 years after observational discovery)
Authors: G S Bisnovatyi-Kogan
Comments: Physics-Uspekhi 49 (1)53-61 (2006)

Bol'shoi obzor po radio pul'saram, raskruchennym za schet akkrecii v tesnyh dvoinyh sistemah. Obzor dostupen i na russkom na saite UFN.


obzor astro-ph/0611483 Perspektivy rentgenovskoi polyarimetrii i ee vozmozhnoe ispol'zovanie dlya izucheniya neitronnyh zvezd (The prospects for X-ray polarimetry and its potential use for understanding neutron stars)
Authors: M.C. Weisskopf et al.
Comments: 17 pages and 13 figures. Paper presented at the 363-rd Heraeus Seminar in Bad Honef, Germany. The paper will be published as a Springer Lecture Notes.

Poka issledovaniya polyarizacii rentgenovskogo izlucheniya astronomicheskih ob'ektov nahodyatsya v zachatochnom sostoyanii: to avariya (kak s yaponskimi apparatami), to konkurenty zarubyat proekt s horoshim polyarimetrom (kak s nashim SRG). Tem ne menee, rano ili pozdno takoi instrument poyavitsya, vozmozhno dazhe na sputnike s rossiiskim uchastiem (novyi SRG).

V obzore v osnovnom obsuzhdayutsya polyarimetricheskie issledovaniya neitronnyh zvezd. Krome etogo, opisano sostoyanie del so stroyashimisya instrumentami i razvivayushimisya tehnologiyami.


obzor astro-ph/0611589 Kakie zvezdy prevrashayutsya v chernye dyry, a kakie v neitronnye zvezdy? (Which Stars Form Black Holes and Neutron Stars?)
Authors: Michael P. Muno
Comments: 8 pages, 3 figures. Uses aipproc.cls. To appear in the proceedings of the conference ``The Multicoloured Landscape of Compact Objects and their Explosive Origins'', 2006 June 11--24, Cefalu, Sicily, to be published by AIP

Mne stat'ya pokazalas' ochen' interesnoi. V samom dele, my ploho ponimaem, kakie iz massivnyh zvezd prevrashayutsya v neitronnye zvezdy, a kakie v chernye dyry. Yasno tol'ko, chto net kakogo-to odnogo universal'nogo predela na massu, vyshe kotoroi zvezda yavlyaetsya praroditelem chernoi dyry.


astro-ph/0611595 Ogranicheniya na uravnenie sostoyaniya pri vysokoi plotnosti po dannym o kompaktnyh zvezdah (Compact star constraints on the high-density EoS)
Authors: H. Grigorian, D. Blaschke, T. Klahn
Comments: 4 pages, 6 figures

Avtory rassmatrivayut razlichnye podhody, pozvolyayushie po nablyudeniyam neitronnyh zvezd dat' ogranicheniya na uravnenie sostoyaniya veshestva v ih nedrah.


astro-ph/0611680 Raskrutka pul'sarov iz-za neustoichivosti v akkrecionnoi udarnoi volne sverhnovoi (Pulsar spins from an instability in the accretion shock of supernovae)
Authors: John M. Blondin, Anthony Mezzacappa
Comments: To be published in Nature

Opisany rezul'taty chislennogo modelirovaniya vzryva sverhnovoi i ego posledstvii, kotorye, vozmozhno, pozvolyayut prolit' svet na to, kak raskruchivayutsya novorozhdennye neitronnye zvezdy.

Sm. takzhe astro-ph/0611698.


obzor astro-ph/0611708 Povorotnye tochki v evolyucii magnitnogo polya odinochnyh neitronnyh zvezd (Turning Points in the Evolution of Isolated Neutron Stars' Magnetic Fields)
Authors: U. Geppert
Comments: 37 pages and 14 figures. Paper presented (in part) at the 363-rd Heraeus Seminar in Bad Honef, Germany. The paper will be published as a Springer Lecture Notes. Submitted for refereeing

Daetsya obzor evolyucii magnitnogo polya neitronnyh zvezd, nachinaya s samyh pervyh minut ih zhizni.


Vypusk 143. 18-31 oktyabrya 2006

astro-ph/0610685 Magnitar XTE J1810-197: variacii tormozyashego momenta, plotnosti radiopotoka i struktury profilya impul'sa (The magnetar XTE J1810-197: variations in torque, radio flux density and pulse profile morphology)
Authors: F. Camilo et al.
Comments: Submitted to ApJ; 7 pages, 5 figures.

Istochnik XTE J1810-197 otnositsya k anomal'nym rentgenovskim pul'saram (ARP). Odnako on vydelyaetsya sredi nih peremennost'yu svoei aktivnosti, kak govoryat "tranzientnost'yu". Nedavno udalos' poluchit' celyi ryad nablyudenii etogo istochnika v radiodiapazone. Etomu i posvyashena, v osnovnom, stat'ya.

Avtory smogli poluchit' dostatochno dlinnyi (neskol'ko mesyacev) ryad nablyudenii. Pri etom udalos' dostatochno tochno otslezhivat' variacii chastoty vrasheniya, tempa ee izmeneniya, radiopotoka. Krome togo, izmenyalsya profil' impul'sa magnitara.

Osnovnaya ideya sostoit v tom, chtoby sopostavit', kak vse eti izmeneniya korreliruyut drug s drugom, a takzhe s dannymi, poluchennymi v drugih diapazonah (prezhde vsego v rentgenovskom). Tak, naprimer, padenie radiopotoka (kak pikovogo, tak i srednego) sovpalo s umen'sheniem tempa zamedleniya vrasheniya neitronnoi zvezdy. A variacii struktury profilya impul'sa v radiodiapazone ne povliyali na ego sovpadenie (po faze) s rentgenovskim impul'som.

Avtory nadeyutsya (i ya s nimi solidaren), chto takie dannye dolzhny pomoch' prodvinut'sya v ponimanii mehanizma raboty magnitarov.


astro-ph/0610768 vozmozhno magnitarnoi prirode IGR J16358-4726 (A Possible Magnetar Nature for IGR J16358-4726)
Authors: S. K. Patel et al.
Comments: Accepted for publication in ApJ, 34 pgs, 14 figures, 4 tables

Avtory detal'no izuchayut odin iz zhestkih rentgenovskii istochnikov, otkrytyh observatoriei Integral. Vo-pervyh, im udalos' pokazat', chto obnaruzhennyi period - okolo 1.6 chasa - skoree vsego yavlyaetsya periodom vrasheniya neitronnoi zvezdy. Vo-vtoryh, udalos' obnaruzhit' izmenenie perioda, ego umen'shenie. Ono ves'ma veliko i sovpadaet s periodom aktivnosti istochnika. Eto govorit o tom, chto neitronnaya zvezda byla raskruchena akkreciei, a magnitnoe pole samoi neitronnoi zvezdy ves'ma veliko. Poslednee i pozvolyaet avtoram rassuzhdat' o magnitarnoi prirode nablyudaemogo ob'ekta.

Na vsyakii sluchai podcherknu: rech' ne idet o rodstve istochnika s takimi izvestnymi kandidatami v magnitary kak anomal'nye rentgenovskie pul'sary i istochniki myagkih povtoryayushihsya gamma-vspleskov. Rech' prosto idet o neitronnoi zvezde s ochen' bol'shim magnitnym polem, prichem zvezda vhodit v tesnuyu dvoinuyu sistemu. Mne lichno sovsem ne nravitsya upotreblenie termina "magnitar" v takom kontekste. Magnitar - eto, vse-taki, ne prosto neitronnaya zvezda s bol'shim polem, a ob'ekt, ch'ya aktivnost', svyazana s polem. zdes' zhe aktivnost', skoree vsego, svyazana s akkreciei.


astro-ph/0610802 O prirode preryvistogo pul'sara PSR B1931+24: rentgenovskie i opticheskie nablyudeniya (On the nature of the intermittent pulsar PSR B1931+24: X-ray and optical observations)
Authors: N. Rea et al.
Comments: 5 pages, 2 figures; submitted to MNRAS Letter

Ya uzhe pisal ob udivitel'nom pul'sare "na polstavki" PSR B1931+24. V dannoi zhe stat'e avtory predstavlyayut rezul'taty rentgenovskih i opticheskih nablyudenii etogo ob'ekta, a takzhe obsuzhdayut vozmozhnost' interpretacii dannyh.

K sozhaleniyu, rezul'taty nablyudenii otricatel'nye, t.e. uvidet' nichego ne udalos'. Istochnik slishkom slab i v optike, i v rentgene. Avtorskaya interpretaciya sistemy takova: eto dvoinaya s periodom okolo mesyaca i ochen' malomassivnoi normal'noi zvezdai. Periody "vyklyucheniya" radiopul'sara ob'yasnyayutsya vliyaniem veshestva normal'noi zvezdy.

Na moi vzglyad, hotya eto i vpolne vozmozhnyi variant, u avtorov poka net dostatochnyh osnovanii dlya utverzhdenii o dvoistvennosti. Naibolee privlekatel'noi ideei, opyat' zhe na moi vzglyad, ostaetsya gipoteza o tom, chto v sluchae etogo pul'sara my nablyudaem perehod mezhdu rezhimami tokovyh poter' (model' Beskina, Gurevicha, Istomina) i magnito-dipol'nymi poteryami (sm. astro-ph/0608689).


astro-ph/0610840 Magnitovrashatel'nyi kollaps massivnyh zvezdnyh yader v neitronnye zvezdy: modelirovanie s uchetom effektov OTO (Magnetorotational collapse of massive stellar cores to neutron stars: Simulations in full general relativity)
Authors: Masaru Shibata, Yuk Tung Liu, Stuart L. Shapiro, Branson C. Stephens
Comments: 28 pages, 20 figures, accepted for publication in Phys. Rev. D

Porazitel'no vse-taki slozhnaya shtuka - vzryv sverhnovoi!

Vot ocherednoi raschet. V nem avtory pytayutsya uchest' rol' magnitnyh polei. Rezul'taty sravnivayutsya s drugimi modelyami i podhodami.


Vypusk 142. 01-18 oktyabrya 2006

obzor astro-ph/0610304 Nedavnii progress v issledovanii anomal'nyh rentgenovskih pul'sarov (Recent Progress on Anomalous X-ray Pulsars)
Authors: V.M. Kaspi
Comments: 10 pages

Zamechatel'nyi obzor po issledovaniyu anomal'nyh rentgenovskih pul'sarov (ARP). Novostei tam mnogo: issledovanie tranzientnyh pul'sarov, vspyshki ARP, obnaruzhenie zhestkih "hvostov" v spektre. V obshem, rezul'tatov mnogo - chitaite.


Vypusk 141. 15-30 sentyabrya 2006

astro-ph/0609544 O vozmozhnosti identifikacii korotkogo/zhestkogo vspleska GRB 051103 s gigantskoi vspyshkoi MPG v gruppe galaktik vokrug M81 (On the Possibility of Identification of a Short/Hard Burst GRB 051103 with the Giant Flare from a Soft Gamma Repeater in the M81 Group of Galaxies)
Authors: D.D. Frederiks, et al.
Comments: 11 pages, 4 figures, accepted for publication in Astronomy Letters

MPG - eto istochniki myagkih povtoryayushihsya gamma-vspleskov. V nashei Galaktike ih izvestno tri, plyus eshe odin v Magellanovom oblake, plyus est' kandidaty. Inogda eti istochniki dayut moshnye, t.n. gigantskie, vspyshki. Po svoim svoistvam oni pohozhi na korotkie gamma-vspleski (kotorye, veroyatnee vsego svyazany so sliyaniyami neitronnyh zvezd). Konechno, kosmicheskie gamma-vspleski moshnee gigantskih vspyshek, no vremennye i spektral'nye svoistva ochen' blizki. Poetomu vspyshku magnitara v ne ochen' dalekoi galaktike mozhno pereputat' s korotkim gamma-vspleskom.

V stat'e avtory opisyvayut nablyudeniya vspleska GRB 051103. Na nebe on popadaet v oblast', gde nahoditsya izvestnaya galaktika M81. Sootvetstvenno, voznikaet mysl' o tom, chto my mozhem videt' gigantskuyu vspyshku magnitara. Avtory polagayut, chto tak ono i est'.

K takim zhe vyvodam prihodyat v svoei stat'e Ofek i dr.

Podrobnee ob etom otkrytii mozhno prochest' v ANKe Dnya na saite Elementy.Ru ili zdes'.

Obsudit' v ZhZh-soobshestve ru_astroph.
Obsudit' na Astroforume v Nauchnoi panorame.


Vypusk 140. 01-15 sentyabrya 2006

astro-ph/0609416 Obrazovanie dvoinogo pul'sara PSR J0737-3039A/B (The Formation of the Double Pulsar PSR J0737-3039A/B)
Authors: I. H. Stairs, et al.
Comments: To appear in MNRAS Letters

Otkrytie dvoinogo radiopul'sara stalo vazhnym rezul'tatov dlya ryada napravlenii.
1. Nalichie takogo ob'ekta pozvolyaet issledovat' vazhnye effekty, imeyushie mesto v pul'sarnyh magnitosferah (napomnyu, chto okonchatel'noi teorii magnitosfer pul'sarov tak i net).
2. Obnaruzhenie takogo ob'ekta pozvolilo povysit' "nablyudatel'nyi" predel na kolichestvo sliyavayushihsya dvoinyh neitronnyh zvezd, chto vazhno dlya ocenki effektivnosti raboty detektorov gravitacionnyh voln. Krome togo, ocenka tempa sliyanii po nablyudaemym sistemam, sostoyashim iz dvuh neitronnyh zvezd, nakonec-to stala sovpadat' s raschetami metodom populyacionnogo sinteza.
3. Dvoinoi radiopul'sar otkryvaet novye vozmozhnosti dlya proverki Obshei teorii otnositel'nosti (sm. ssylku nizhe).
4.Nalichie takogo ob'ekta brosaet vyzov teoriyam evolyucii zvezd.
Poslednemu punktu i posvyashena stat'ya.

Delo v tom, chto:
1. U pul'sara nizkaya prostranstvennaya skorost'. T.e., ne bylo bol'shogo kika (bol'shogo dopolnitel'nogo impul'sa pri vzryve sverhnovoi)
2. U sistemy nizkii, no nenulevoi, ekscentrisitet orbity.
3. Sistema imeet dovol'no korotkii orbital'nyi period.
Vse vmeste eto stavit problemy v postroenii evolyucionnogo scenariya, privedshego k poyavleniyu takoi sistemy. Odin iz vazhnyh vyvodov sostoit v tom, chto predsverhnovaya, porodivshaya bolee molodoi pul'sar (pul'sar V), imela nizkuyu massu, okolo 2 mass Solnca ili dazhe men'she. T.o. vryad li eto byla obychnaya sverhnovaya s kollapsom zheleznogo yadra. S drugoi storony, pohozhaya dvoinaya sistema PSR B1534+12 po vsei vidimosti imela nekol'ko inuyu istoriyu. T.o., vozmozhny raznye evolyucionnye puti, chto nado uchityvat' v modelyah, opisyvayushih poyavlenie takih sistem.

Sm. takzhe stat'yu astro-ph/0609417 toi zhe gruppy avtorov, v kotoroi rassmatrivayutsya testy OTO po dannym o dvoinom pul'sare.


Vypusk 139. 01-31 avgusta 2006

astro-ph/0608205 Pryamoe izmerenie skorosti otdachi neitronnoi zvezdy v kislorodnom ostatke sverhnovoi Puppis A (Direct Measurement of Neutron-Star Recoil in the Oxygen-Rich Supernova Remnant Puppis A)
Authors: P. Frank Winkler, Robert Petre
Comments: 18 pages

Po sobstvennomu dvizheniyu udalos' opredelit' skorost' neitronnoi zvezdy v ostatke sverhnovoi Puppis A. Skorost' ochen' velika: 1500 km/s. V principe, takie skorosti uzhe izmeryalis' u neitronnyh zvezd (radiopul'sarov). Tem ne menee, eto primechatel'nyi rezul'tat. Poyasnyu pochemu.

Neitronnaya zvezda v Puppis A prinadlezhit k klassu t.n. central'nyh kompaktnyh ob'ektov. Eto molodye neitronnye zvezdy, nablyudaemye v ostatkah sverhnovyh, no pri etom ne proyavlyayushie nikakoi radiopul'sarnoi aktivnosti. Nablyudayut ih v rentgenovskom diapazone za schet teplovogo izlucheniya goryachei poverhnosti kompaktnogo ob'ekta. Hotya takih neitronnyh zvezd izvestno vsego neskol'ko shtuk, no ih molodost' privodit k ocenke chastoty rozhdeniya poryadka chastoty poyavleniya na svet obychnyh radiopul'sarov. Pochemu znachitel'naya chast' neitronnyh zvezd rozhdaetsya stol' nepohozhimi na privychnye radiopul'sary ostaetsya zagadkoi. V svyazi s etim opredelenie skorosti dlya odnogo iz ob'ektov dannogo tipa predstavlyaet bol'shoi interes.

Novost' ob etom otkrytii mozhno takzhe prochest' na Granyah.Ru.


astro-ph/0608225 Obzor 56-ti oblastei lokalizacii istochnikov EGRET dlya poiska radiopul'sarov (A Survey of 56 Mid-latitude EGRET Error Boxes for Radio Pulsars)
Authors: F. Crawford, et al.
Comments: 24 pages, including 4 figures and 3 tables. Accepted for publication in ApJ

EGRET - eto odin iz gamma-detektorov na bortu CGRO. Podavlyayushee bol'shinstvo istochnikov, zaregistrirovannyh etim priborom, ostaetsya neotozhdestvlennym. Schitaetsya, chto est' tri osnovnye sostavlyayushie. Vo-pervyh, eto vnegalakticheskie istochniki (aktivnye yadra galaktik, v osnovnom, vidimo, blazary). Oni raspredeleny ravnomerno po nebesnoi sfere. Vo-vtoryh, eto istochniki v diske Galaktiki. Nakonec, est' eshe populyaciya, svyazannaya s Poyasom Gulda. Raschety pokazyvali, chto v Poyase dolzhno byt' mnogo radiopul'sarov, kotorye i dali by neobhodimyi gamma-potok (otmechu, chto odna iz novyh populyacii neitronnyh zvezd - Velikolepnaya semerka - tochno svyazana s Poyasom). Avtory stat'i proveli special'nyi poisk radiopul'sarov v oblastyah lokalizacii neotozhdestvlennyh istochnikov EGRET, polozhenie kotoryh na nebe mozhet govorit' o vozmozhnoi svyazi s Poyasom Gulda.

Rezul'taty poiska okazalis' otricatel'nymi. Nesmotrya na obnaruzhenie neskol'kih novyh pul'sarov net ni odnogo, kotoryi mozhno bylo by svyazat' s kakim-to iz gamma-istochnikov. Avtory polagayut, chto ocenki chisla radiopul'sarov v Poyase Gulda byli slishkom optimistichnymi.

Ya lichno polagayu, chto istochniki taki dolzhny byt' svyazany s odinochnymi molodymi neitronnymi zvezdami v Poyase Gulda. Otkrytiya poslednih let uzhe priuchili nas k tomu, chto molodye neitronnye zvezdy vovse ne obyazatel'no dolzhny proyavlyat' obychnuyu radiopul'sarnuyu aktivnost'. Zapusk sputnika GLAST privedet k tomu, chto koordinaty gamma-istochnikov budut opredeleny gorazdo tochnee. Nuzhno budet tshatel'no poiskat' v novyh oblastyah lokalizacii neitronnye zvezdy.


astro-ph/0608311 Chandra chuet RRAT (Chandra Smells a RRAT: X-ray Detection of a Rotating Radio Transient)
Authors: B.M. Gaensler et al.
Comments: 5 pages, 2 b/w figures, 1 color figure. To appear in the proceedings of "Isolated Neutron Stars", Astrophysics & Space Science, in press

Eto stat'ya, napravlennaya v materialy aprel'skoi londonskoi konferencii po neitronnym zvezdam. V nei rasskazyvaetsya ob obnaruzhenii v dannyh Chandra odnogo iz RRATs (napomnyu, chto eto novyi tip neitronnyh zvezd, obnaruzhennyi po tranzientnoi aktivnosti v radiodiapazone). Ya uzhe rasskazyval ob etom otkrytii, no ne greh i vtoroi raz ego pomyanut'. Odnako, stat'ya vklyuchena v obzory iz-za odnoi vazhnoi, na moi vzglyad, detali. Na stranice 4 v razdele 5 avtory pishut, chto seichas idet proekt AstroPulse, v ramkah kotorogo idet poisk radiotranzientov po rezul'tatam programmy SETI@home. Eto horosho ukladyvaetsya v koncepciyu o tom, chto astronomicheskie nablyudeniya po programma SETI mogut rabotat' vmeste. Hotya na moi vzglyad logichnee, esli SETI pol'uzuetsya rezul'tatami astronablyudenii, a ne naoborot.


miniobzor astro-ph/0608345 Kvarkovoe veshestvo v neitronnyh zvezdah (Quark Matter in Neutron Stars: An apercu)
Authors: Prashanth Jaikumar, Sanjay Reddy, Andrew W. Steiner
Comments: 15 pages, 1 figure. Invited review for Modern Physics Letters A

Ochen' tolkovyi obzor po kvarkovym zvezdam. Nichego supernovogo, no ochen' yasno napisano i ohvachen shirokii krug imenno astrofizicheskih voprosov.

Vtoroi, bolee detal'nyi, obzor mozhno naiti zdes': astro-ph/0608360.


Vypusk 138. 01-31 iyulya 2006

astro-ph/0607173 Dolgoperiodicheskii sil'no peremennyi rentgenovskii istochnik v molodom ostatke sverhnovoi (A long-period, violently-variable X-ray source in a young SNR)
Authors: A. De Luca, P.A. Caraveo, S. Mereghetti, A. Tiengo, G.F. Bignami
Comments: Accepted for publication in Science. Published online via Science Express on 2006, July 6. 17 pages, 7 figures

Kompaktnyi istochnik v ostatke sverhnovoi RCW 103 izvesten uzhe dostatochno davno. Tak zhe davno bylo yasno, chto on ne pohozh na "normal'nuyu" moloduyu neitronnuyu zvezdu. Vyskazyvalis' samye raznye gipotezy. Peremennost' istochnika, v svoyu ochered', tozhe ne yavlyaetsya novost'yu. I dazhe periodichnost' peremennosti uzhe obsuzhdalas', naprimer v rabotah G.G.Pavlova i ego kolleg. I vse-taki vot on - gvozd': detal'nye nablyudeniya na HMM-N'yutone pokazali nalichie chetkoi periodichnosti s periodom 6.67 chasa.

Priroda istochnika po-prezhnemu ostaetsya neponyatnoi. To li eto dvoinaya sistema s malomassivnym kompan'onom (prisutstvie kompan'ona nikak v drugih diapazonah ne proyavlyaetsya), to li eto odinochnaya neitronnaya zvezda s anomal'no bol'shim (dlya takogo molodogo ob'ekta) periodom vrasheniya, to li chto-to eshe. Ne mogu ne vspomnit' svoyu staruyu ideyu o tom, chto istochnik yavlyaetsya "staroi" neitronnoi zvezdoi, a sam ostatok porozhden vzryvom kompan'ona po dvoinoi sisteme. Teper' zhe "staraya" neitronnaya zvezda akkreciruet vybroshennoe veshestvo. Pravda, period v chetvert' dnya tut takzhe ploho podhodit (pri takom periode orbital'naya skorost' slishkom velika, chtoby ozhidat' znachimoi akkrecii iz sredy vokrug). Mozhno postroit' model' v duhe "epiciklov", skazav, chto iznachal'no imelas' troinaya sistema (dve massivnye zvezdy i odna malomassivnaya). Massivnaya zvezda, vzrvavshayasya vtoroi, porodila nablyudaemyi ostatok, a pervaya porodila akkreciruyushuyu neitronnuyu zvezdu. Kak by to ni bylo, polagayu, chto ne stoit sbrasyvat' so schetov vozmozhnost', chto v kachestve rentgenovskogo istochnika my vidim ne tu zhe neitronnuyu zvezdu, chto porodila ostatok. Budem dumat' i zhdat'.


astro-ph/0607528 >Rentgenovskii spektr 10.6-sekundnogo pul'sara v Westerlund 1 po dannym Chandra" proverka magnitarnoi gipotezy (The Chandra X-ray Spectrum of the 10.6 s Pulsar in Westerlund 1: Testing the Magnetar Hypothesis)
Authors: S.L. Skinner, R. Perna, S.A. Zhekov
Comments: 20 pages, 5 figures; to appear in ApJ

Proveden analiz dannyh rentgenovskih nablyudenii odnogo iz anomal'nyh rentgenovskih pul'sarov, nahodyashegosya v skoplenii Westerlund 1. Hotya po "pervichnym priznakam" ob'ekt pohozh na standartnye anomal'nye pul'sary, tem ne menee polnoi yasnosti net. Svetyat ochen' malen'kie "pyatna", i polnaya svetimost' pri etom na poryadok men'she, chem u drugih istochnikov dannogo tipa.


astro-ph/0607614 Poisk pul'sacii v radiodiapazone ot chetyreh anomal'nyh rentgenovskih pul'sarov i otkrytie dvuh novyh pul'sarov (Search for radio pulsations in four Anomalous X-ray Pulsars and discovery of two new pulsars)
Authors: M. Burgay et al.
Comments: 8 pages, 6 figures, accepted by MNRAS

Avtory proveli poisk pul'siruyushego radioizlucheniya ot chetyreh anomal'nyh rentgenovskih pul'sarov: 1RXS J170849.0-400910, 1E1048.1-5937, 1E 1841-045, AX J1845-0258. Ni ot odnogo ne bylo obnaruzheno radioimpul'sov. Zato poputno udalos' otkryt' dva novyh radiopul'sara!

Poisk provodilsya na vysokoi chastote (okolo 1300 MGc). Mozhet byt' v etom kroetsya prichina neudachi. Ved' poka zhe polozhitel'nogo rezul'taty udalos' dostich' tol'ko gruppe issledovatelei v Pushino, kotorye ot anomal'nogo rentgenovskogo pul'sara 1E 2259+586 smogli zaregistrirovat' pul'siruyushee radioizluchenie na nizkoi chastote (okolo 110 MGc). [Da eshe ot ARP XTE 1810-197 udalos' uvidet' radioizluchenie vo vremya aktivnoi fazy istochnika astro-ph/0605429]


astro-ph/0607640 Parksovskii mnogopuchkovyi obzor neba. VI. Otkrytie i taiming 142 pul'sarov i populyacionnyi sintez galakticheskih pul'sarov (The Parkes multibeam pulsar survey: VI. Discovery and timing of 142 pulsars and a Galactic population analysis)
Authors: D. R. Lorimer et al.
Comments: 30 pages, 8 figures, 9 tables, accepted for publication in MNRAS

Vo-pervyh, avtory opisyvayut svezheotkrytye pul'sary. Ih azh 142. T.o., polnoe chislo pul'sarov, otkrytyh v ramkah obzora, dostiglo 742!!! Vo-vtoryh, ispol'zuya polnye dannye po pul'saram, zadetektirovannym v ramkah proekta, avtory vychislyayut vazhnye parametry populyacii vcelom. V chastnosti temp rozhdeniya pul'sarov sostavlyaet 1.4+/-0.2 za sto let.


Vypusk 137. 16 iyunya - 30 iyunya 2006

astro-ph/0606465 Otkrytie dvuh pul'sarov v napravlenii galakticheskogo centra (Discovery of two pulsars towards the Galactic Centre)
Authors: Simon Johnston, M. Kramer, D. R. Lorimer, A. G. Lyne, M. McLaughlin, B. Klein, R. N. Manchester
Comments: 5 pages, Submitted to MNRAS Letters

Sushestvuet takaya problema: zvezd v oblasti galakticheskogo centra mnogo, v tom chisle i molodyh, a vot s pul'sarami - napryazhenka. Byli dazhe otdel'nye raboty, pokazyvavshie nedostatok pul'sarov vblizi centra Galaktiki (rech' idet o central'nyh sotnyah parsek). A vot raportuyut ob otkrytii dvuh istochnikov, kotorye po vsei vidimosti raspolozheny na 150-500 pk ot centra.


astro-ph/0606524 Kvarkovoe veshestvo i massy-radiusy kompaktnyh zvezd (Quark matter and the masses and radii of compact stars)
Authors: Mark Alford et al.
Comments: 3 pages, LaTeX

V nedavnei stat'e astro-ph/0605106 byl proveden analiz dannyh po neitronnoi zvezde v tesnoi dvoinoi rentgenovskoi sisteme EXO 0748-676. Vyvod avtora sostoyal v tom, chto t.n. myagkie uravneniya sostoyaniya veshestva kompaktnoi zvezdy mozhno otvergnut'. Stalo byt', razvivala etu mysl' avtor, mozhno zakryt' i kvarkovye zvezdy. Odnako avtory dannoi stat'i pokazyvayut, chto vyvod, sdelannyi v stat'e astro-ph/0605106, yavlyaetsya slishkom sil'nym obobsheniem, ibo mnogie sovremennye modeli kvarkovyh zvezd imeyut dovol'no zhestkoe uravnenie sostoyaniya. T.o., polagayut avtory stat'i, ocenki massy i radiusa EXO 0748-676 ne protivorechat gipoteze kvarkovyh zvezd.


obzor astro-ph/0606674 Fizika sil'nozamagnichennyh neitronnyh zvezd (Physics of Strongly Magnetized Neutron Stars)
Authors: Alice K. Harding, Dong Lai
Comments: 93 pages. Reports on Progress in Physics, in press (2006)

Otlichnyi bol'shoi obzor po neitronnym zvezdam s sil'nym magnitnym polem. Osnovnoe vnimanie udelyaetsya teorii, sobstvenno, avtory i yavlyayutsya teoretikami.

Vazhnyi moment sostoit v tom, chto pri roste magnitnogo polya proishodit "perehod kolichestva v kachestvo". Est' nekotorye kriticheskie znacheniya polya, pri kotoryh sushestvennymi stanovyatsya processy, ne idushie (ili ochen' maloeffektivnye) pri men'shih polyah. Samoe vazhnoe kriticheskoe znachenie - 4.4 1013 Gauss. Eto t.n. Shvingerovskoe pole. V takom pole ciklotronnaya energiya elektrona stanovitsya ravnoi ego energii pokoya.

Takie polya - eto ne pridumka teoretikov. Tochnee, eto bylo pridumkoi. A seichas my znaem bolee dyuzhiny neitronnyh zvezd, ocenki polei v kotoryh dayut znacheniya, prevyshayushie shvingerovskoe.


miniobzor astro-ph/0606732 Nablyudeniya neitronnyh zvezd na Chandre (Chandra X-Ray Observatory Observations of Neutron Stars: An Overview)
Authors: M. C. Weisskopf, M. Karovska, G. G. Pavlov, , V. E. Zavlin, T. Clarke
Comments: 10 pages, 14 figures. Submitted to Astronomy and Space Science. Based on presentation at Isolated Neutron Stars, London, 2006

Postepenno nachinayut poyavlyat'sya materialy prekrasnoi konferencii po odinochnym neitronnym zvezdam, proshedshei v aprele v Londone.

Kak yasno iz nazvaniya, rech' idet o vklade Chandry v issledovaniya etih ob'ektov: central'nyh kompaktnyh ob'ektov v ostatkah sverhnovyh, radiopul'sarov, ob'ektov Velikolepnoi semerki. Vazhen dazhe otricatel'nyi rezul'tat: avtory special'no opisyvayut vazhnye verhnie predely, poluchennye na Chandre, dlya vozmozhnoi neitronnoi zvezdy v ostatke sverhnovoi 1987A i v gamma Lebedya (SNR 78.2+2.1).


Vypusk 136. 01 iyunya - 15 iyunya 2006

obzor astro-ph/0606017 Vysokoenergichnoe izluchenie pul'sarnyh magnitosfer (High-energy Emission from Pulsar Magnetospheres)
Authors: Kouichi Hirotani
Comments: 16 pages, 9 figures, Mod. Phys. Lett. A in press

Neplohoi obzor po magnitosfernomu izlucheniyu pul'sarov v diapazone rentgenovskih i gamma-luchei. Seichas v preddverii zapuskov sputnikov AGILE i GLAST eto vse ves'ma aktual'no.


astro-ph/0606027 Rasstoyaniya do anomal'nyh rentgenovskih pul'sarov, opredelennye po krasnym zvezdam (Distances to Anomalous X-ray Pulsars using Red Clump Stars)
Authors: Martin Durant, Marten H. van Kerkwijk
Comments: 38 pages aastex, 10 figures. Accepted for publication in ApJ

Zagolovok, kak vy obratili vnimanie, pereveden ne vpolne tochno, t.k. ya prosto ne znayu ustoyavshegosya russkogo termina dlya red clump stars, a predlozhenie svoego varianta - delo dovol'no otvetstvennoe i trebuet razdumiya. Itak ...

Izmerenie rasstoyanii do anomal'nyh rentgenovskih pul'sarov (ARP) yavlyaetsya ochen' neprostym delom. Neprostym, no vazhnym. Avtory ispol'zovali infrakrasnye dannnye po zvezdam, nablyudayushimsya v napravleniyah na izvestnye ARP. Vmeste s dannymi o pogloshenii v rentgenovskom diapazone, poluchaemymi nepostredstvenno iz nablyudenii ARP, eta informaciya pozvolila avtoram utochnit' rasstoyaniya do ARP. Vo-pervyh, podtverzhdeno, chto ARP nahodyatsya v spiral'nyh rukavah. Eto horosho, no eshe ne supervazhno. Vo-vtoryh, i eto uzhe teplee, svetimosti ARP okazalis' ochen' blizkimi - poryadka 10 v 35 stepeni erg za sekundu. Nakonec, i eto samoe vazhnoe, obnaruzhena ochen' horoshaya antikorrelyaciya radiusa chernotel'no izluchayushei oblasti ("goryachego pyatna") s dolei pul'siruyushego izlucheniya. Takzhe vidna nekotoraya antikorrelyaciya radiusa goryachego pyatna s temperaturoi. Vse eto ochen' vazhno dlya postroeniya modeli ARP, kotoraya poka taki otsutstvuet.


astro-ph/0606345 Yavlyaetsya li pul'sar B0656+14 ochen' blizkim RRAT? (Is pulsar B0656+14 a very nearby RRAT source?)
Authors: P. Weltevrede, B.W. Stappers, J.M. Rankin, G.A.E. Wright
Comments: 4 pages, 4 figures, accepted by ApJL

Napomnyu, chto RRATs - Rotating Radio Transients - eto novyi tip neitronnyh zvezd, obnaruzhennyi menee goda nazad po ochen' korotkim vspyshka v radiodiapazone. Chto eto za neitronnye zvezdy, s kakimi izvestnymi tipami etih kompaktnyh ob'ektov oni svyazany (i svyazany li voobshe) - neizvestno.

Avtory stat'i raportuyut ob obnaruzhenii pohozhih vspyshek u blizkogo pul'sara B0656+14. Esli by etot istochnik, pishut avtory, nahodilsya na rasstoyanii centra Galaktiki, to vse, chto my videli by eto samye moshnye impul'sy, ispyskaemye im. Prichem harakteristiki etih impul'sov byli by ochen' pohozhi na harakteristiki, nablyudaemyh vspyshek RRATs. Drugih pohozhih pul'sarov poka ne obnaruzheno. Bezuslovno, nuzhny novye nablyudeniya.


Vypusk 135. 22 aprelya - 31 maya 2006

astro-ph/0604562 Korotkie gamma-vspleski ot sliyaniya dvoinyh neitronnyh zvezd (Short Gamma-Ray Bursts from Binary Neutron Star Mergers)
Authors: Roland Oechslin, Thomas Janka
Comments: 6 pages, 2 figures, Proceedings of the Albert Einstein Century International Conference, Paris, France, 2005, edited by Jean-Michel Alimi and Andre Fuzfa

Modelirovat' sliyaniya neitronnyh zvezd voobshe slozhno. Esli zhe v dobavok interesuet, kak vse eto budet svetit' v gamma-diapazone, to zadacha stanovitsya eshe slozhnee. Na moi vzglyad, poka programmy nedostatochno sovershenny, chtoby davat' chetkie detal'nye odnoznachnye otvety, no progress nalico.


astro-ph/0604605 Pul'sar s periodicheskoi aktivnost'yu daet dannye o magnitosfernoi fizike (A periodically active pulsar giving insight into magnetospheric physics)
Authors: M. Kramer et al.
Comments: 12 pages, 2 figures; Science 312 (2006) 549-551

Pul'sar PSR B1931+24 (J1933+2421) obladaet interesnym povedeniem: v techenie neskol'kih dnei on svetit kak obychnyi pul'sar, a potom na neskol'ko nedel' vyklyuchaetsya. Kogda on nahoditsya v aktivnom sostoyanii, to temp ego zamedleniya v dva raza vyshe, chem kogda on vyklyuchen.

Iz razgovorov so specialistami ya ponyal, chto oni vozlagayut bol'shie nadezhdy na etot pul'sar. Veroyatnee vsego on mozhet sygrat' rol' rozetskogo kamnya. Imeya dannye o tempe zamedleniya v aktivnom i passivnom sostoyaniyah, my mozhem sudit' o tokah, tekushih v magnitosfere pul'sara, chto yavlyaetsya kriticheskim voprosom dlya konkuriruyushih teorii pul'sarnyh magnitosfer. Ili, mozhno skazat', chto etot pul'sar stanet lakmusovoi bumazhkoi. Ibo v nekotoryh teoriyah opisat' takoe povedenie mozhno, a v nekotoryh - nel'zya.


astro-ph/0605154 Priroda gigantskih impul'sov radiopul'sarov (Nature of giant pulses in radio pulsars)
Authors: S. A. Petrova
Comments: 8 pages, 2 figures. Invited review for the 2005 Hanas Lake International Pulsar Symposium, to appear in ChJAA

Kak izvestno, u pul'sarov, krome obychnyh, nablyudayutsya eshe i t.n. gigantskie impul'sy. Proishozhdenie etogo fenomena neyasno. V stat'e privoditsya odna iz gipotez, ob'yasnyayushaya gigantskie impul'sy.


astro-ph/0605330 Infrakrasnoe otozhdestvlenie magnitara 1RXS J170849.0-400910 (The infrared counterpart to the magnetar 1RXS J170849.0-400910)
Authors: Martin Durant, Marten H. van Kerkwijk
Comments: 19 pages AASTEX, 4 figure. Accepted for publication in ApJ.

Proveden novyi analiz infrakrasnyh dannyh po odnomu iz anomal'nyh rentgenovskih pul'sarov. Vidimo, ob'ekt, kotoryi ran'she schitalsya infrakrasnym istochnikom, svyazannym s magnitarom, takovym ne yavlyaetsya.


astro-ph/0605331 Evolyuciya zamagnichennyh neitronnyh zvezd s differencial'nym vrasheniem: modelirovanie s polnym uchetom effektov OTO (Evolution of magnetized, differentially rotating neutron stars: Simulations in full general relativity)
Authors: Matthew D. Duez et al.
Comments: 27 pages, 30 figures; Journal-ref: Phys. Rev. D73 (2006) 104015

Privodyatsya rezul'taty chislennogo modelirovaniya povedeniya molodyh neitronnyh zvezd s uchetom mnogih detalei.


astro-ph/0605429 Tranzientnoe pul'siruyushee radioizluchenie magnitara (Transient pulsed radio emission from a magnetar)
Authors: Fernando Camilo et al.
Comments: 6 pages, 2 figures. Submitted to Nature

Otkryto pul'siruyushee radioizluchenie ot odnogo iz anomal'nyh rentgenovskih pul'sarov. Esli ranee lish' Pushinskim gruppam udavalos' uvidet' radioizluchenie ot t.n. radiotihih neitronnyh zvezd (anomal'nye rentgenovskie pul'sary, istochniki myagkih povtoryayushihsya gamma-vspleskov, Velikolepnaya semerka) v nizkochastotnom diapazone, to teper' i v standartnom pul'sarnom diapazone udalos' koe-chto razglyadet'!


astro-ph/0605449 Magnitary kak ostyvayushie neitronnye zvezdy s vnutrennim podogrevom (Magnetars as cooling neutron stars with internal heating)
Authors: A.D. Kaminker et al.
Comments: 8 pages, 5 figures, submitted to MNRAS

Izuchaetsya teplovaya evolyuciya magnitarov. Avtory polagayut, chto u magnitarov dolzhen byt' kakoi-to istochnik dopolnitel'nogo podogreva vo vneshnih sloyah.


Vypusk 134. 12-21 aprelya 2006

astro-ph/0604288 Parksovskaya pul'sarnaya vremennaya reshetka (The Parkes Pulsar Timing Array)
Authors: R N Manchester
Comments: 10 pages, in press ChJAA

Konechno, hochetsya zaregistrirovat' gravitacionnye volny kak mozhno neposredstvennee. Dlya etogo i stroyat lazernye interferometry i tverdotel'nye ustanovki. Odnako nablyudeniya radiopul'sarov pozvolyayut poluchat' dannye o gravitacionnyh volnah pust' i ne stol' neposredstvennym, zato bolee deshevym putem. Vse horosho znayut o tom, chto dvoinye radiopul'sary ispytyvayut izmeneniya orbit za schet izlucheniya gravitacionnyh voln. Est' i drugie effekty, svyazannye s nablyudeniem etih ob'ektov, pozvolyayushie poluchat' informaciyu o gravitacionnyh volnah.

Vazhnym dostoinstvom millisekundnyh radiopul'sarov yavlyaetsya porazitel'naya ustoichivost' ih periodov. Ona sravnima s luchshimi zemnymi atomnymi chasami. Po suti, nablyudeniya neskol'kih takih pul'sarov mogut dat' standart chastoty prevoshodyashii atomnye! Etu osobennost' mozhno ispol'zovat' dlya kosvennogo nablyudeniya garvitacionnyh voln.

Gravitacionnye volny vliyayut na nablyudaemye periody pul'sarov. Imenno na nablyudaemye, t.k. rech' idet ob effekte, svyazannym s prohozhdeniem volny cherez nas. Iz-za prohozhdeniya volny period pul'sara budet kazat'sya nam to koroche, to dlinnee. Ideya takogo obnaruzheniya gravitacionnyh voln byla vpervye vyskazana M.V. Sazhinym v 1978 g. Issleduya odin ob'ekt mozhno dat' verhnii predel na fon gravitacionnyh voln (vokrug nas) v opredelennom diapazone chastot. Prichem, pul'sarnye dannye chuvstvitel'ny k ochen' bol'shim periodam - poryadka vremeni nablyudeniya, t.e. neskol'ko let (sootvetstvenno, chastoty gravvoln ischislyayutsya v dannom sluchae nanogercami). Nablyudeniya za neskol'kimi pul'sarami pozvolyaet (tochnee mozhet pozvolit') zaregistrirovat' etot gravitacionno-volnovoi fon.

Sobstvenno, "pul'sarnaya vremennaya reshetka" (Pulsar Timing Array) eto ne novyi pribor. Sami pul'sary i obrazuyut "reshetku" ili "set'". Nablyudeniya zhe planiruetsya provodit' na uzhe horosho izvestnom 64-metrovom radioteleskope. Hotya, elektronnaya nachinka i programmnoe obespechenie dolzhny byt' dorabotany, chtoby vyiti na neobhodimuyu chuvstvitel'nost'. Takaya neobhodimost' byla prodemonstrirovana v techenie pervogo goda nablyudenii.

O proekte takzhe mozhno pochitat' zdes'.


astro-ph/0604421 Otkrytie 14 radiopul'sarov v obzore Magellanovyh oblakov (Discovery of 14 radio pulsars in a survey of the Magellanic Clouds)
Authors: R N Manchester, G Fan, A G Lyne, V M Kaspi
Comments: 20 pages, In press, ApJ

S pomosh'yu novoi apparatury na 64-metrovom radioteleskope v Avstralii proveden poisk radiopul'sarov v Magellanovyh oblakah. Obnaruzheno 14 novyh ob'ektov. 2 iz nih po vsei vidimosti prinadlezhat nashei Galaktike (t.e. oni prosto sluchaino proeciruyutsya na Oblaka), a vot 12 nahodyatsya v samih sputnikah Mlechnogo Puti. 9 - v Bol'shom Magellanovom oblake, i 3 - v Malom. Chtoby ocenit' mnogo eto ili malo otkryt' 12 novyh radiopul'sarov v etih karlikovyh galaktikah, skazhu tol'ko, chto ranee tam bylo izvestno vsego 8 radiopul'sarov.

Odnako, nikakih supersensacii ne proizoshlo. Otkrytye pul'sary dovol'no zauryadny. Tem ne menee, progress nalico. Uchityvaya, chto, naprimer, Maloe Magellanovo oblako otlichaetsya ot nashei Galaktiki men'shei metallichnost'yu, budet interesno uznat', okazyvaet li eto vliyanie na pul'sarnuyu populyaciyu. Dlya takogo analiza neobhodimo obnaruzhit' bol'shee kolichestvo radiopul'sarov. Budem zhdat' novyh otkrytii.


obzor astro-ph/0604422 Strannost' v neitronnyh zvezdah (Strangeness in Neutron Stars)
Authors: Fridolin Weber, et al.
Comments: 16 pages, 5 figures, 3 tables; Accepted for publication in the Proceedings of the International Workshop on Astronomy and Relativistic Astrophysics (IWARA) 2005, Int. J. Mod. Phys. D

Esli chut' vyshe ya rasskazyval o rabote, posvyashennoi belym karlikam, to v etoi stat'e vy naidete dostatochno polnyi obzor po strannym neitronnym zvezdam. Chast' obzora prednaznachena dlya specialistov. Tem ne menee, chast' napisana dostatochno dostupno, i ona posluzhit horoshim dopolneniem k stat'e po strannym belym karlikam.


Vypusk 133. 01-11 aprelya 2006

astro-ph/0604076 Ostatochnyi disk vokrug molodoi odinochnoi neitronnoi zvezdy (A Debris Disk Around An Isolated Young Neutron Star)
Authors: Zhongxiang Wang, Deepto Chakrabarty, David L. Kaplan
Comments: 5 pages, 3 figures. To appear in Nature (6 Apr 2006)

Ochen' vazhnoe otkrytie, o kotorom ya uslyshal eshe v avguste na konferencii v Vankuvere. Odnako, v Nature strogoe recenzirovanie, i, vidimo, avtoram prishlos' pomuchit'sya.

Po dannym infrakrasnyh nablyudenii na Spitcere obnaruzhen disk vokrug odnogo iz anomal'nyh rentgenovskih pul'sarov (4U 0142+61). Disk legkii (okolo 10 mass Zemli). On ne sushestvenen v smysle akkrecii na neitronnuyu zvezdu. My vidim disk lish' potomu, chto on osveshaetsya potokom rentgenovskih luchei ot anomal'nogo pul'sara. To, chto eto disk, a ne obolochka, dokazyvaetsya tem, chto obolochka s takimi zhe infrakrasnymi harakteristikami, davala by slishkom bol'shoe pogloshenie v rentgenovskom i opticheskom diapazonah, chto ne nablyudaetsya. Disk dostatochno daleko otstoit ot neitronnoi zvezdy. Vnutrennii radius granicy diska sostyavlyaet neskol'ko radiusov Solnca, t.e. bolee milliona kilometrov (radius samoi neitronnoi zvezdy - okolo 10 km).

Takie diski estestvennym obrazom dolzhny voznikat' v processe t.n. "obratnoi akkrecii" (fallback) posle vzryva sverhnovoi, kogda chast' veshestva ne uletaet "na beskonechnost'", a ili vypadaet obratno na neitronnuyu zvezdu, ili ostaetsya vrashat'sya vokrug nee v vide diska.

Anomal'nye rentgenovskie pul'sary schitayutsya kandidatami v magnitary - sil'no zamagnichennye neitronnye zvezdy, rashoduyushie energiyu etogo polya. Dannoe otkrytie vo mnogom podderzhivaet etu gipotezu, t.k. okonchatel'no zakryvaet odnu iz al'ternativ - teoriyu, v kotoroi rol' istochnika energii igraet moshnyi disk vokrug neitronnoi zvezdy (ob etom mozhno koe-chto posmotret', naprimer, v moei prezentacii "Zoopark neitronnyh zvezd").

Infrakrasnye dannye est' eshe dlya treh anomal'nyh rentgenovskih pul'sarov. No tam oni (poka) ne stol' detal'ny. Mozhno ozhidat', chto takie ostatochnye diski yavlyayutsya obshim svoistvom etogo klassa odinochnyh neitronnyh zvezd. Bylo by interesno posmotret', mogut li takie diski perezhit' period stol' burnoi aktivnosti, kak te, chto nablyudayutsya i istochnikov myagkih povtoryayushihsya gamma-vspleskov. Esli okazhetsya, chto ne mogut, to togda anomal'nye rentgenovskie pul'sary ne yavlyayutsya "starshimi brat'yami" (t.e. sleduyushei evolyucionnoi stadiei) istochnikov myagkih povtoryayushihsya gamma-vspleskov. Krome togo, interesno posmotret', perezhil li by takoi disk stadiyu sushestvovaniya sverhzamagnichennoi bystrovrashayusheisya neitronnoi zvezdy. Esli net, to eto bylo by argumentom v pol'zu togo, chto magnitary poyavlyayutsya uzhe dovol'no medlenno vrashayushimisya. Eto vazhno dlya vyyasneniya mehanizm proishozhdeniya magnitnogo polya, t.k. dlya generacii ego s pomosh'yu dinamo-mehanizma bystroe vrashenie absolyutno neobhodimo. Tak ili inache, no otkrytie etogo diska ochen' vazhno dlya vsei magnitarnoi astrofiziki, a takzhe dlya fiziki sverhnovyh.

Takzhe poyavilas' stat'ya, posvyashennaya poisku pyli vokrug radiopul'sara PSR 1257+12. Iskali tozhe s pomosh'yu Spitcera. Rezul'tat otricatel'nyi. Stoit otmetit', chto v etom sluchae meshaet izluchenie samogo pul'sara, poetomu dazhe poyas, tipa nashego poyasa Koipera, ne udalos' by rassmotret'.


astro-ph/0604187 Energetika ostatkov sverhnovyh i magnitary: otsutstvie ukazanii v pol'zu protoneitronnyh zvezd s millisekundnymi periodami (Supernova remnant energetics and magnetars: no evidence in favour of millisecond proto-neutron stars)
Authors: Jacco Vink, Lucien Kuiper
Comments: Accepted for publication in MNRAS Letters. 5 pages, one color figure

Interesnaya rabota. Logika avtorov takova. Esli magnitnye polya magnitarov generiruyutsya na stadii protoneitronnoi zvezdy, to mozhno poiskat' posledstviya etogo. Vo vseh mehanizmah generacii ispol'zuetsya ochen' bystroe vrashenei protoneitronnoi zvezdy. Neobhodimy periody koroche primerno 30 millisekund (obratite vnimanie, rech' idet o protoneitronnoi zvezde, ona menee kompaktna, chem uzhe ostyvshaya prorelaksirovavshaya neitronnaya zvezda, poetomu 30 millisekund dlya nee eto ochen' korotkii period!). Esli my posmotrim na neitronnuyu zvezdu so stol' korotkim periodom i sil'nym polem, to uvidim, chto eto kolossal'nyi izluchatel'! Takoi vprysk energii mozhet (dolzhen!) ostavit' sled na ostatke sverhnovoi.

Avtory analiziruyut dannye po neskol'kim ostatkam sverhnovyh, v kotoryh nahodyatsya magnitary. Vyvod ih sostoit v tom, chto nikakih sledov vpryska energii ne vidno. A znachit, zaklyuchayut oni, polya magnitarov ne mogut generirovat'sya s pomosh'yu obsuzhdaemyh dinamo-mehanizmov. V etom sluchae oni, naprimer, mogut predstavlyat' ostatochnye polya zvezd-praroditelei. Togda magnitary rozhdayutsya uzhe s medlennym vrasheniem i bol'shimi polyami.

Otmechu, chto poslednee slovo tut eshe ne skazano. U gipotezy ob ostatochnyh polyah tozhe est' svoi problemy: vryad li est' stol'ko zvezd s sil'nymi polyami, chtoby ob'yasnit' vse magnitary. V konce koncov, sama koncepciya magnitarov - eto gipoteza.


Vypusk 132. 22-31 marta 2006

astro-ph/0603845 Sozdanie ul'trasil'nyh magnitnyh polei pri sliyanii neitronnyh zvezd (Producing ultra-strong magnetic fields in neutron star mergers)
Authors: Daniel Price, Stephan Rosswog
Comments: 14 pages, 4 figures, accepted to Science.

Pokazano, chto v rezul'tate sliyaniya dvuh neitronnyh zvezd iz-za razvitiya neustoichivosti Kel'vina-Gel'mgol'ca mogut voznikat' ochen' sil'nye magnitnye polya. Oni mogut prevoshodit' polya magnitarov, s kotorymi svyazyvayut povtoryayushiesya myagkie gamma-vspleski. Avtory polagayut, chto obnaruzhennaya osobennost' mozhet pozvolit' ob'yasnit' korotkie gamma-vspleski.

(Napomnyu, chto v proshlom godu byli polucheny sushestvenneishie nablyudatel'nye argumenty v pol'zu togo, chto korotkie gamma-vspleski svyazany so sliyaniyami kompaktnyh ob'ektov.)


Vypusk 130. 01-13 marta 2006

astro-ph/0603089 Gigantskie impul'sy - osnovnoi komponent radioizlucheniya pul'sara v Krabe (Giant Pulses -- the Main Component of the Radio Emission of the Crab Pulsar)
Authors: M.V. Popov et al.
Comments: 13 pages, 6 figures (originally published in Russian in Astronomicheskii Zhurnal, 2006, vol. 83, No. 1, pp. 62-69) translated by Denise Gabuzda; Journal-ref: Astronomy Reports, 2006, vol. 50, No. 1, pp. 55-61

Ya, sobstvenno, slyshal doklad po etoi rabote na seminare Gurevicha v FIANe. Ochen' interesnaya rabota (i ochen' horoshii doklad). Tak vot, sut' v tom, chto to, chto my seichas nazyvaem kak "obychnye" impul'sy pul'sara v Krabe, sut' gigantskie impul'sy. A v samom dele "obychnye" impul'sy u etogo pul'sara nablyudayutsya kak t.n. prekursor.

Fraza vyshe bezuslovno maloponyatnaya, poetomu s udovol'stviem raz'yasnyu. U radiopul'sarov nablyudayut razlichnye tipy impul'sov. Po vsei vidimosti, s nimi svyazany raznye mehanizmy izlucheniya. Dlya nas seichas budut vazhny "obychnye" i "gigantskie" impul'sy. Obychnost', kak obychno, sootvetstvuet vysokoi chastote vstrechaemosti. Gigantizm, ochevidno, govorit o tom, chto etot tip impul'sov byl otkryt blagodarya nablyudeniyu ochen' moshnyh sobytii. Tshatel'nyi analiz pul'sara v Krabe pokazal, chto vo-pervyh, gigantskie impul'sy poyavlyayutsya tol'ko na teh fazah, na kotoryh vidno bol'shinstvo impul'sov. Vo-vtoryh, raspredelenie impul'sov po energii edino dlya vseh impul'sov na sootvetstvuyushih fazah. Eto pozvolyaet skazat', chto vse impul'sy na etih fazah sleduet otnosit' k gigantskim nevziraya na ih moshnost'. A gde zhe normal'nye impul'sy? Oni tozhe est', no na drugih fazah. U pul'sara v Krabe est' t.n. prekursor. Eto impul's pered osnovnym pul'som. Po vsei vidimosti, imenno prekursor i sostoit iz obychnyh impul'sov.

T.o., gigantskie impul'sy ne yavlyayutsya kakim-to redkim sobytiem. Mehanizm, otvetstvennyi za nih, vovsyu rabotaet (po-krainei mere u pul'sara v Krabe). Specialisty po pul'saram ochen' pozitivno ocenivayut etot rezul'tat. Vozmozhno, chto on pozvolit sushestvenno prodvinut'sya v ponimanii togo, kak svetyat radiopul'sary.


astro-ph/0603147 Nestacionarnaya bessilovaya magnitosfera pul'sara: osesimmetrichnye i naklonnye rotatory (Time-dependent force-free pulsar magnetospheres: axisymmetric and oblique rotators)
Authors: Anatoly Spitkovsky
Comments: Submitted to ApJ Letters

Nesmotrya na to, chto radiopul'sary izvestny uzhe pochti 40 let, mehanizm ih izlucheniya ostaetsya zagadkoi. V poslednie godu novoe pokolenie uchenyh predprinimaet novuyu ataku na dannuyu problemu, ispol'zuya, v osnovnom, chislennyi podhod. Odna iz takih popytok predstavlena v dannoi stat'e.

Drugoi variant izlozheniya toi zhe raboty mozhno naiti v stat'e astro-ph/0603212. Eto 6-tistranichnye trudy konferencii (gde ya, kstati, s Anatoliem i poznakomilsya). Vozmozhno, chto komu-to kratkii variant ponravitsya bol'she.


Vypusk 129. 20-28 fevralya 2006

astro-ph/0602501 Opticheskaya registraciya dvuh kompan'onov pul'sarov v dvoinyh sistemah promezhutochnyh mass (Optical Detection of Two Intermediate Mass Binary Pulsar Companions)
Authors: B. A. Jacoby et al.
Comments: 9 pages, 2 figures, accepted for publication in ApJL

Na krupnom nazemnom teleskope v observatorii im. Magellana avtory proveli poisk opticheskogo izlucheniya ot shesti belyh karlikov, yavlyayushihsya kompan'onami radiopul'sarov. Ne vse eti pul'sary yavlyayutsya millisekundnymi. Odin - vpolne normal'nyi molodoi pul'sar (PSR J1141-6545). No uvidet' belyi karlik v optike udalos' tol'ko v dvuh sluchayah, i vo vseh nih kompan'onom yavlyaetsya millisekundnyi pul'sar. Oba etih sluchaya vydelyaet to, chto oni nahodyatsya dovol'no blizko ot nas (menee 1 kpk), tak chto bolee glubokie nablyudeniya mogut potom dat' polozhitel'nyi rezul'tat i dlya drugih sistem.

Vse eto ochen' vazhno, t.k. dlya belyh karlikov mozhno opredelyat' vozrast, esli izvestna ih temperatura (i massa).


Vypusk 128. 13-20 fevralya 2006

obzor astro-ph/0602234 Neustoichivosti vrashayushihsya kompaktnyh zvezd: kratkii obzor (Instabilities of rotating compact stars: a brief overview)
Authors: L. Villain
Comments: 19 pages, Proceeding of Cargese School "Astrophysical fluid dynamics" (May 2005) organized by B. Dubrulle and M. Rieutord in honour of J.-P. Zahn and S. Bonazzola

Podrobnyi, ponyatnyi i interesnyi obzor, posvyashennyi neustoichivostyam v neitronnyh zvezdah i rodstvennyh im ob'ektah. Takie neustoichivosti budut privodit' k generacii gravitacionnyh voln. Otsyuda termin "gravitacionno-volnovaya astroseismologiya". Pravda, registraciya takih kolebanii - delo budushego.


astro-ph/0602359 Magnitary kak postoyannye istochniki zhestkogo rentgena: Otkrytie zhestkogo hvosta u SGR 1900+14 na Integrale (Magnetars as persistent hard X-ray sources: INTEGRAL discovery of a hard tail in SGR 1900+14)
Authors: D. Gotz, S. Mereghetti, A. Tiengo, P. Esposito
Comments: 5 pages, 2 figures, submitted to A&A Letters

Sputnik Integral horosh ne tol'ko tem, chto on rabotaet v ochen' zhestkom rentgenovskom diapazone, gde do nego takih instrumentov ne bylo. Horosh on eshe i tem, chto, obladaya shirokim polem zreniya, on pozvolyaet poluchat' ochen' dlitel'nye ekspozicii, osobenno dlya istochnikov, lezhashih v oblasti galakticheskogo centra. Tak vot, po dannym 2.5 millionov sekund nablyudenii (!) otkryto postoyannoe zhestkoe izluchenie ot odnogo iz MPG - SGR 1900+14.

Sushestvennym otkrytiem avtorov stalo to, chto anomal'nye rentgenovskie pul'sary sushestvenno otlichayutsya ot MPG v zhestkom diapazone spektra (1-100 keV).


Vypusk 127. 01-12 fevralya 2006

obzor astro-ph/0602047 Strannost' v kompaktnyh zvezdah (Strangeness in Compact Stars)
Authors: Fridolin Weber
Comments: 26 pages, 13 figures, 29th Johns Hopkins Workshop on current problems in particle theory: Strong Matter in the Heavens

Pod strannost'yu ponimaetsya ne "otkloneniya", a kvantovoe svoistvo "strannost'". V nedrah kompaktnyh zvezd mogut obrazovyvat'sya chasticy, nesushie sootvetstvuyushee kvantovoe chislo. Naibolee izvestnye predstaviteli semeistva - eto t.n. "strannye zvezdy". No rech' idet ne tol'ko o nih, no i ob giperonnyh zvezdah, strannyh karlikah i t.p.


Vypusk 125. 18-20 yanvarya 2006

astro-ph/0601357 Izmerenie mer vrasheniya pul'sarov i krupnomasshtabnaya struktura galakticheskogo magnitnogo polya (Pulsar rotation measures and the large-scale structure of Galactic magnetic field)
Authors: J.L. Han et al.
Comments: ApJ accepted. 16 pages, 14 figures, 2 tables, 223 pulsar RMs

Po dannym o mere vrasheniya pul'sarov (eto ne nechto, svyazannoe s vrasheniem samih neitronnyh zvezd, eta velichina pokazyvaet kak izmenilas' orientaciya ploskosti polyarizacii izluchennoi pul'sarov elektromagnitnoi volny po mere ee rasprostraneniya ot istochnika k priemniku) mozhno izuchat' strukturu magnitnogo polya Galaktiki. Avtory na osnove izmereniya mer vrasheniya dlya 223 radiopul'srov poluchayut kartinu global'nogo magnitnogo polya nashei zvezdnoi sistemy.


Na risunke pokazano napravlenie magnitnogo polya v Galaktike po dannym o mere vrasheniya pul'sarov.


Vypusk 125. 18-20 yanvarya 2006

astro-ph/0601357 Izmerenie mer vrasheniya pul'sarov i krupnomasshtabnaya struktura galakticheskogo magnitnogo polya (Pulsar rotation measures and the large-scale structure of Galactic magnetic field)
Authors: J.L. Han et al.
Comments: ApJ accepted. 16 pages, 14 figures, 2 tables, 223 pulsar RMs

Po dannym o mere vrasheniya pul'sarov (eto ne nechto, svyazannoe s vrasheniem samih neitronnyh zvezd, eta velichina pokazyvaet kak izmenilas' orientaciya ploskosti polyarizacii izluchennoi pul'sarov elektromagnitnoi volny po mere ee rasprostraneniya ot istochnika k priemniku) mozhno izuchat' strukturu magnitnogo polya Galaktiki. Avtory na osnove izmereniya mer vrasheniya dlya 223 radiopul'srov poluchayut kartinu global'nogo magnitnogo polya nashei zvezdnoi sistemy.


Na risunke pokazano napravlenie magnitnogo polya v Galaktike po dannym o mere vrasheniya pul'sarov.


Vypusk 123. 24-31 dekabrya 2005

astro-ph/0512585 Rozhdenie i evolyuciya odinochnyh radiopul'sarov (Birth and Evolution of Isolated Radio Pulsars)
Authors: C.-A. Faucher-Giguere, V. M. Kaspi
Comments: 73 preprint pages, including 8 tables and 15 figures. ApJ submission revised following the referee's comments

Populyacionnye issledovaniya pul'sarov ochen' vazhny i aktual'ny. Krome togo, ih neobhodimo regulyarno nezavisimo povtoryat', t.k. postoyanno rastet statistika i nahodyatsya kakie-to novye svoistva.

V rabote predstavleno detal'noe chislennoe modelirovanie populyacii radiopul'sarov v nashei Galaktike. Po rezul'tatam avtorov poluchaetsya, chto temp rozhdeniya nemnogo (v poltora raza) vyshe, chem poluchalos' v bolee rannih rabotah. Vse mozhno ob'yasnit' bez zatuhaniya magnitnogo polya, a skorosti mogut imet' odnomodovoe, no ne maksvellovskoe raspredelenie.


astro-ph/0512630 Registraciya na RHESSI vysokochastotnyh rentgenovskih oscillyacii v hvoste gipervspyshki SGR 1806-20 (Detection with RHESSI of high frequency X-ray oscillations in the tail of the 2004 hyperflare from SGR 1806-20)
Authors: Anna L Watts, Tod E Strohmayer
Comments: 5 pages, 5 figures using emulateapj. Accepted for publication in ApJ Letters

Ya uzhe rasskazyval ob otkrytii oscillyacii v hvostah gigantskih vspyshek. Te oscillyacii sootvetstvovali chastotam okolo 90 Gc. Teper' zhe obnaruzheny bolee vysokochastotnye na 600 Gc. S chem svyazany eti kolebaniya neyasno.


astro-ph/0512643 G359.95-0.04: kandidat v pul'sary ryadom s Sgr A* (G359.95-0.04: Pulsar Candidate Near Sgr A*)
Authors: Q. D. Wang et al.
Comments: 11 pages, accepted for publication in MNRAS

Po rentgenovskim nablyudeniya v neposredstvennoi blizosti ot centra nashei Galaktiki obnaruzhena tumannost', kotoruyu avtory identificiruyut kak pul'sarnuyu tumannost'.

Istochnik nahoditsya vsego v treti parseka ot Sgr A* (konechno, rech' idet o proekcii). V principe, nalichie pul'sara v central'noi oblasti Galaktiki ne dolzhno udivlyat', t.k. tam polno massivnyh zvezd (Sergei Nayakshin delal ochen' interesnyi doklad na etu temu na nedavnei konferencii NEA-2005, prohodivshei v IKI). Tem ne menee, my otmechaem eto otkrytie, poskol'ku eto pervoe ukazanie na nalichie radiopul'sara stol' blizko ot centra Galaktiki.


nucl-th/0512098 Ogranicheniya na ostyvanie neitronnyh zvezd dlya sluchaya cvetnoi sverhprovodimosti gibridnyh zvezd (Neutron star cooling constraints for color superconductivity in hybrid stars)
Authors: S. Popov, H. Grigorian, D. Blaschke
Comments: 10 pages, 9 figures, 1 table

God zakonchen. Mozhno pozvolit' sebe vol'nost'. Poslednei stat'ei 2005 goda v obzorah budet nasha poslednyaya rabota, posvyashennaya ostyvaniyu neitronnyh zvezd.

V 2004 godu nami byl predlozhen novyi test krivyh ostyvaniya neitronnyh zvezd. Togda my oprobovali ego na nabore krivyh ostyvaniya obychnyh neitronnyh zvezd (poluchilos', chto test rabotaet neploho, sovsem skoro v Astronomy & Astrophysics vyidet stat'ya na etu temu). Teper' my prilozhili nash test k gibridnym zvezdam.

Ne budu vlezat' v detali, a rasskazhu ob odnoi sushestvennoi idee, kotoruyu my popytalis' takzhe razvit' v etoi novoi stat'e. Rech' idet o tom, chto, ob'yasnyaya dannye nablyudenii s pomosh'yu teoreticheskih krivyh ostyvaniya, nado pomnit' o spektre mass neitronnyh zvezd. Obychno, massivnye zvezdy ostyvayut bystree. I inogda teoretiki stremyatsya provesti cherez samye holodnye iz izvestnyh neitronnyh zvezd krivye, sootvetstvuyushie samym massivnym. Na nash vzglyad, eto neverno. Delo v tom, chto massivnyh neitronnyh zvezd malo. Teoreticheskie raschety (naprimer, v rabotah gruppy Vusli) pokazyvayut, chto novorozhdennyh neitronnyh zvezd s massoi bolee 1.4-1.5 solnechnyh dolzhno byt' malo (neskol'ko procentov). T.o., maloveroyatno, chto sredi dyuzhiny neitronnyh zvezd s izvestnoi temperaturoi i vozrastom my vidim predstavitelei etogo massivnogo men'shinstva.

Vot i vse. Eshe raz vseh s proshedshimi prazdnikami. S nailuchshimi pozhelaniyami

Sergei.

Vypusk 122. 11-23 dekabrya 2005

astro-ph/0512379 Otkrytie rentgenovskogo izlucheniya ot radiotranzienta J1819--1458 (Discovery of the X-ray Counterpart to the Rotating Radio Transient J1819--1458)
Authors: S.P. Reynolds et al.
Comments: 4 pages, 2 figures, submitted to ApJL

Ya podrobno rasskazyval ob otkrytii novogo tipa neitronnyh zvezd (sm. zdes' i zdes'). I vot - novaya novost'.

Odin iz novyh istochnikov sluchaino popal v pole zreniya Chandry vesnoi etogo goda. Analiz pokazal nalichie rentgenovskogo istochnika. T.k. Chandra daet dostatochno tochnye koordinaty, to udalos' pokazat', chto ni v optike, ni v IK tam nichego ne vidno. Eto podtverzhdaet gipotezu o tom, chto my imeem delo s odinochnoi neitronnoi zvezdoi. Mne lichno takzhe ochen' radostno, chto novye dannye sovmestimy s gipotezoi o teplovom izluchenii neitronnoi zvezdy. Togda, v samom dele, eto mogut byt' ob'ekty tipa Velikolepnoi semerki.


Vypusk 120. 12-30 noyabrya 2005

astro-ph/0511523 Molodoi relyativistskii dvoinoi pul'sar J1906+0746 (The young, highly relativistic binary pulsar J1906+0746)
Authors: D. Lorimer et al.
Comments: 19 pages, 3 figures, accepted for publication in ApJ

Otkryt interesnyi (i, vidimo, vazhnyi) dvoinoi pul'sar. Delo v tom, chto eto, po vsei vidimosti, ocherednaya sistema, sostoyashaya iz dvuh neitronnyh zvezd (al'ternativa - sistema s OChEN' massivnym belym karlikom). Pochemu otkrytie budet ochen' vazhnym, esli eto podtverditsya?

Vo-pervyh, eto ochen' vazhno dlya ocenki tempa sliyaniya neitronnyh zvezd. Sam otkrytyi pul'sar - eto molodoi ob'ekt. Ocenki pokazyvayut, chto sistema sol'etsya vsego lish' cherez 0.3 milliarda let. Eto podtverzhdaet vysokii temp sliyanii neitronnyh zvezd v Galaktike.

Vo-vtoryh,(i eto interesno lichno mne) massa sistemy ocenivaetsya v 2.6-2.65 massy Solnca. Esli schitat', chto massy komponent primerno ravny, to poluchaetsya, chto neitronye zvezdy rodilis' s massami <1.4 massy Solnca. Eto uzhe vos'maya sistema, gde tochno izmereny massy obeih komponent. Vo vseh sistemah dlya zvezd, na kotorye ne bylo sushestvennoi akkrecii (t.e. oni ne mogli sushestvenno uvelichit' svoyu massu posle rozhdeniya), nachal'nye massy men'she 1.4 mass Solnca. Lichnyi interes zaklyuchaetsya v tom, chto t.o. moya ocenka spektra nachal'nyh mass neitronnyh zvezd v okrestnostyah solnca, kotoryi my ispol'zuem v populyacionno sinteze, poluchaet sushestvennoe nablyudatel'noe podtverzhdenie.


astro-ph/0511587 Tranzientnye radio vspyshki ot vrashayushihsya neitronnyh zvezd (Transient radio bursts from rotating neutron stars)
Authors: M. A. McLaughlin et al.
Comments: 10 pages, 4 figures. Accepted by Nature

Nakonec-to poyavilas' stat'ya (opyat'-taki, prinyataya v Nature), posvyashennaya otkrytiyu tranzientnyh radioistochnikov. Poskol'ku ya pisal ob etom paru mesyacev nazad, to ogranichus' lish' ssylkoi na dostatochno polnoe opisanie otkrytiya: /elementy.ru/news/164793.

Ot sebya dobavlyu eshe, chto mogut byt' raznye gipotezy o proishozhdenii istochnikov. Na osnovanii dannyh o periodah i ih proizvodnyh avtory iznachal'no obsuzhdali vozmozhnoe rodstvo s magnitarami. V final'noi versii stat'i poyavilos' uzhe i upominanie o Velikolepnoi semerke (sam ya sklonyayus' poka imenno k takomu mneniyu). V samom dele, iz vseh izvestnyh populyacii neitronnyh zvezd Velikolepnaya semerka vo-pervyh, luchshe vseh podhodit po periodam i proizvodnym, a vo-vtoryh, (i eto ochen' vazhno) ob'ekty tipa Velikolepnoi semerki dolzhny byt' ochen' mnogochislenny (my vidim poka lish' samye blizkie i molodye). T.e. eto edinstvennyi izvestnyi tip neitronnyh zvezd, kotoryi podhodit dlya ob'yasneniya radiotranzientov s tochki zreniya tempa rozhdeniya. Tem ne menee, upomyanu eshe odnu vozmozhnost', kotoraya poka ne obsuzhdalas'. Ocenka chisla radiotranzientov v Galaktike daet chislo poryadka 400 000. Eto gde-to 0.1% ot polnogo chisla neitronnyh zvezd. Siya velichina prekrasno soglasuetsya s ocenkoi chisla sverhzvukovyh propellerov, sdelannoi v nashei rabote v 2000 godu (astro-ph/9910114). Novye ocenki Beskina i Eliseevoi (astro-ph/0508442) pokazali, chto propellery mogut poyavlyat'sya i s dostatochno korotkimi periodami. T.o. ne isklyucheno, chto novyi tip istochnikov mozhet byt' svyazan i s propellerami. Periody nemnogo korotkovaty, no eto mozhet byt' svyazano s bolee slabym magnitnym polem.


astro-ph/0511783 Rentgenovskoe i infrakrasnoe uyarchenie anomal'nogo rentgenovskogo pul'sara 1E 2259+58 (X-Ray and Infrared Enhancement of Anomalous X-ray Pulsar 1E 2259+58)
Authors: U. Ertan, E. Gogus, M. A. Alpar
Comments: 17 pages, 3 figures, accepted for publication in ApJ

Avtory pytayutsya interpretirovat' dannye rentgenovskih i IK nablyudenii odnogo iz anomal'nyh rentgenovskih pul'sarov, ispol'zuya model' ostatochnogo diska. Takie struktury mogut obrazovyvat'sya iz-za obratnogo vypadaniya (fall-back) chasti veshestva, vybroshennogo pri vzryve sverhnovoi. Po slovam avtorov, im udaetsya opisat' nablyudaemye yavleniya v ramkah svoei modeli. Otmechu, odnako, chto na moi vzglyad stroit' otdel'nuyu model' dlya ARP, ignoriruya istochniki myagkih povtoryayushihsya gamma-vspleskov, vryad li produktivno. A vspleski diskom ne ob'yasnit'.


Vypusk 119. 29 oktyabrya - 11 noyabrya 2005

astro-ph/0511068 Gravitacionnoe izluchenie ot novorozhdennyh magnitarov (Gravitational Radiation from Newborn Magnetars)
Authors: Luigi Stella et al.
Comments: 5 pages, Accepted for publication on ApJ Letters

Ya uzhe pisal nedavno o rabote, svyazannoi s gravitacionnym izlucheniem magnitarov. Vot eshe odna. Zdes' rech' idet ne o fone, a ob izluchenii ot skopleniya v Deve. V samom dele, tam temp rozhdeniya magnitarov dolzhen byt' dostatochno vysok, a avtory pokazyvayut, chto pri nachal'nom pole poryadka 1016.5 Gs gravitacionno-volnovi signal budet dostatochno silen, chtoby istochnik udalos' uvidet' modernizirovannoi versiei LIGO. Nalichie signala svyazano s tem, chto moshnoe magnitnoe pole deformiruet neitronnuyu zvezdu, i ona stanovitsya istochnikom gravitacionnyh voln (zvezda budet nesimmetrichna otnositel'no osi vrasheniya iz-za magnitnoi deformacii, sootvestvenno vozniknet precessiya). Ocenki pokazyvayut, chto temp rozhdeniya magnitarov v skoplenii v Deve dolzhen byt' poryadka shtuki v god. T.o., esli predpolozhenie o bystrom nachal'nom vrashenii magnitarov i o tom, chto pri rozhdenii ih pole dostigaet 1016.5 Gs, verno, to modernizirovannaya ustanovka LIGO budet videt' odin vsplesk v god, chto nemalo. Otmechu, odnako, chto izbytka gamma vspleskov magnitarov ot etogo skopleni galaktik my ne vidim.


astro-ph/0511084 Opredelenie vremennyh parametrov dlya blizkoi odinochnoi neitronnoi zvezdy RX J1308.6+2127/RBS 1223 (A Coherent Timing Solution for the Nearby Isolated Neutron Star RX J1308.6+2127/RBS 1223)
Authors: D. L. Kaplan, M. H. van Kerkwijk
Comments: 5 pages, 2 figures. ApJL in press

V rabote privedeny dannye po tochnomu opredeleniyu tempa zamedleniya i drugih parametrov dlya odnoi iz zvezd, sostavlyayushih Velikolepnuyu semerku. Novye dannye zadayut i novye voprosy. Naprimer, vozrast istochnika, opredelennyi po tempu zamedleniya sushestvenno vyshe, chem vozrast, opredelennyi po temperature. Znachit, ili neitronnaya zvezda rodilas' s periodom poryadka 7-8 sekund, ili zhe ran'she ona gorazdo bystree zamedlyalas'.


astro-ph/0511142 Kollaps gipermassivnoi zamagnichennoi neitronnoi zvezdy: central'naya mashina dlya korotkih gamma-vspleskov (Magnetized hypermassive neutron star collapse: a central engine for short gamma-ray bursts)
Authors: Masaru Shibata et al.
Comments: 4 pages, 2 figures, submitted to Phys. Rev. Letter

V proshlom vypuske ya uzhe pisal o pervoi rabote etoi gruppy avtorov. Imi rassmatrivaetsya kollaps bystrovrashayusheisya massivnoi zamagnichennoi neitronno zvezdy, obrazovavsheisya v reuzl'tate sliyaniya dvuh neitronnyh zvezd. V predydushei stat'e avtorami lish' kratko byla otmechena vozmozhnost' generacii korotkogo gamma-vspleska pri takom kollapse. V etoi zhe stat'e modelirovanie vspelska yavlyaetsya osnovnoi temoi.


obzor astro-ph/0511258 Dvoinye i millisekundnye pul'sary (Binary and Millisecond Pulsars)
Authors: D.R. Lorimer
Comments: 77 pages, 30 figures, Living Rev. Relativity 8, (2005), 7

Kogda-to ya uzhe rasskazyval o zamechatel'nom proekte Living Reviews on Relativity. Eto setevoi obzornyi zhurnal, publikuyushii obzory po sootvetstvuyushei tematike. Vazhno, chto periodicheski avtory vykladyvayut obnovlennye versii svoih obzorov. Nastoyashaya stat'ya kak raz yavlyaetsya ocherednym primerom. Dunkan Lorimer vylozhil novuyu versiyu svoego obzora po dvoinym i millisekundnym pul'saram. Pozhalui, eto samyi polnyi obzor po teme.


Vypusk 117. 01-17 oktyabrya 2005

astro-ph/0510011 Zatmeniya i modulyacii s orbital'nym periodom v dvoinom pul'sare PSR J0737-3039 (Eclipses and orbital modulations in binary pulsar PSR J0737-3039)
Authors: Maxim Lyutikov
Comments: 10 pages, 3 figures, solicited talk, topical session on PSR J0737-3039, A life with stars, a meeting in honor of Ed van den Heuvel

Predstavlena fenomenologicheskaya model' dvoinogo pul'sara J0737-3039. Za schet togo, chto sistema s dvumya aktivnymi pul'sarami nablyudaetsya nami fakticheski s rebra, udaetsya registrirovat' ochen' interesnye variacii potokov izlucheniya ot pul'sarov. V ramkah prostoi modeli prakticheski vse eti variacii udaetsya ob'yasnit'.


astro-ph/0510018 Gamma vspleski i perehod k kvarkovoi materii v kvarkovyh zvezdah (Gamma Ray Bursts and the transition to Quark Matter in Compact Stars)
Authors: A. Drago et al.
Comments: 4 pages, 1 figure, Proceedings QM2005, August 2005 Budapest

Odnoi iz modelei gamma-vspleska yavlyaetsya perehod veshestva neitronnoi zvezdy v kvarkovoe sostoyanie. T.k., soglasno gipoteze Bodmera-Vittena imenno kvarkovoe veshestvo yavlyaetsya energeticheski bolee vygodnym, to pri takom perehode budet za korotkoe vremya vydelena gigantskaya energiya. Avtory obsuzhdayut osnovnye svoistva takoi modeli i sravnivayut ee s nablyudeniyami.


Vypusk 116. 11 sentyabrya - 30 sentyabrya 2005

astro-ph/0509408 Neitronnaya zvezda s massivnym praroditelem v skoplenii Westerlund 1 (A Neutron Star with a Massive Progenitor in Westerlund 1)
Authors: M. P. Muno et al.
Comments: 4 pages, 4 figures. Submitted to ApJL

V zvezdnom skoplenii Westerlund 1 (na risunke) otkryt anomal'nyi rentgenovskii pul'sar (ARP). Napomnim, chto soglasno sovremennym predstavleniyam ARP - eto molodaya neitronnaya zvezda s sil'nym magnitnym polem. Seichas izvestno uzhe 8 takih ob'ektov plyus est' neskol'ko kandidatov. Chto primechatel'nogo v etom otkrytii? Interesno to, chto Westerlund1 - eto ochen' molodoe skoplenie, v kotorom lish' samye massivnye zvezdy uspeli zakonchit' svoi evolyucionnyi put'. T.o. poluchaetsya, chto praroditelem novogo ARP byla zvezda s nachal'noi massoi okolo 40 mass Solnca. Eto podtverzhdaet gipotezu o tom, chto ARP (i magnitary voobshe) rozhdayutsya iz samyh massivnyh zvezd iz chisla teh, chto eshe porozhdayut neitronnuyu zvezdu, a ne chernuyu dyru.


astro-ph/0509484 Kiki dvoinyh i odinochnyh neitronnyh zvezd: nablyudatel'nye ogranicheniya i prilozheniya k mehanizmu kika (Neutron Star Kicks in Isolated and Binary Pulsars: Observational Constraints and Implications for Kick Mechanisms)
Authors: Chen Wang, Dong Lai, JinLin Han
Comments: 30 pages, 2 figures, submitted to ApJ on Aug. 24, 2005

Kak izvestno, pri rozhdenii neitronnye zvezdy priobretayut znachitel'nuyu prostranstvennuyu skorost' za schet kika (kick - udar, tolchok). Mehanizm kika do sih por ne izvesten. On mozhet byt' svyazan kak s gidrodinamikoi protoneitronnoi zvezdy, tak i s ee magnitnym polem. Krome togo, predlozhen ryad bolee ekzoticheskih mehanizmov (naprimer, bol'shie skorosti mogli by priobretat'sya v sluchae obrazovaniya kvarkovoi zvezdy).

Avtory stat'i obrashayut osoboe vnimanie na to, kak seichas napravlen vektor skorosti neitronnoi zvezdy otnositel'no osi ee vrasheniya. Osnovnoi vyvod avtorov takov: harakternoe vremya kika - poryadka odnoi sekundy. T.e. imenno za eto vremya neitronnaya zvezda nabiraet skorost'. Sootvetstvenno, esli period vrasheniya neitronnoi zvezdy byl menee 1 sekundy, to dva vektora budut pochti sonapravleny. Esli zhe period vrasheniya prevoshodit sekundu, to napravleniya osi vrasheniya i vektora skorosti sovpadat' ne budut.


astro-ph/0509732 Obzor pul'sarov v Aresibo s ispol'zovaniem ALFA. I. Strategiya obzora i pervye otkrytiya (Arecibo Pulsar Survey Using ALFA. I. Survey Strategy and First Discoveries)
Authors: J. M. Cordes et al.
Comments: 10 pp, 9 figures, accepted by the Astrophysical Journal

Predstavleny rezul'taty novogo pul'sarnogo obzora, provodimogo v Aresibo. Uzhe otkryto 11 novyh pul'sarov, sredi nih est' i primechatel'nye. Odin, po vidimomu, svyazan s ranee neotozhdestvlennym gamma-istochnikom, otkrytym priborom EGRET na bortu CGRO. Drugoi nahoditsya v dvoinoi sisteme s korotkim orbital'nym periodom, no pri etom imeet dovol'no bol'shoi period vrasheniya (144 millisekundy). Tretii interesen tem, chto ot nego zaregistrirovany lish' otdel'nye sporadicheskie impul'sy.


astro-ph/0509880 Gravitacionno-volnovoi fon ot magnitarov (Gravitational Wave Background from Magnetars)
Authors: Tania Regimbau, Jos Antonio de Freitas Pacheco
Comments: accepted for publication in A&A 17 pages, 7 figures

Ranee eti avtory uzhe provodili raschety gravitacionno-volnovogo fona, svyazannogo s odinochnymi neitronnymi zvezdami. Delo v tom, chto poskol'ku neitronnye zvezdy slegka nesimmetrichny, oni izluchayut gravitacionnye volny. Izluchayut slabo, no zvezd takih vo vselennoi mnogo. Poetomu summarnyi signal poluchaetsya zametnym, i on mozhet byt' zadetektirovan kak fon. V etoi rabote avtory udelyayut osoboe vnimanie magnitaram. Prichina v tom, chto sil'nye magnitnye polya mogut privodit' k dopolnitel'noi deformacii neitronnoi zvezdy, a takaya zvezda budet sil'nee izluchat'. V proshlyh rabotah etot fakt ignorirovalsya, a zdes' uchten.

Avtory polagayut, chto fon ot magnitarov mozhet v budushem meshat' registracii kosmologicheskih gravitacionnyh voln.

Ot sebya dobavim, chto fon mozhet prihodit' sushestvenno neravnomerno ot raznyh uchastkov neba, t.k. magnitary dolzhny byt' sil'no skoncentrirovany v galaktikah s vysokim tempom zvezdoobrazovaniya. Mozhet byt' etot fakt kak-to pomozhet vychest' magnitarnyi fon.


Vypusk 115. 30 avgusta - 10 sentyabrya 2005

astro-ph/0509031 Poluchaya tychki: VLBA parallaks dlya giperbystrogo pul'sara B1508+55 (Getting Its Kicks: A VLBA Parallax for the Hyperfast Pulsar B1508+55)
Authors: S. Chatterjee et al.
Comments: 5 pages, including 2 figures; Journal-ref: Astrophys.J. 630 (2005) L61-L64

Izvestno, chto pul'sary (da i neitronnye zvezdy voobshe) obladayut bol'shimi prostranstvennymi skorostyami. Impul's priobretaetsya imi v moment rozhdeniya za schet asimmetrii vzryva sverhnovoi. Skorosti mozhno ocenivat' po-raznomu. Naprimer, po forme tumannosti vokrug pul'sara, ili po ego smesheniyu otnositel'no centra ostatka sverhnovoi. No hochetsya, konechno zhe, poluchat' neposredstvennye dannye. Dlya eto nuzhno izmerit' smeshenie pul'sara na nebe (eto legko sdelat') i neobhodimo opredelit' rasstoyanie do pul'sara (a vot eto sdelat' uzhe zatrudnitel'no).

Avtory po dannym VLBA izmerili parallaks pul'sara V1508+55. V rezul'tate udalos' opredelit' skorost' etoi neitronnoi zvezdy. Poluchennoe znachenie - 1083 km/s - okazalos' rekordnym sredi poluchennyh neposredstvennym obrazom.


astro-ph/0509068 Registraciya gigantskih impul'sov ot pul'sara PSR J1752+2359 (Detection of Giant Pulses in pulsar PSR J1752+2359)
Authors: A. A. Ershov, A. D. Kuzmin
Comments: 5 pages, 4 figures, 1 table. Accepted for publication in A&A

Pushinskie radioastronomy zaregistrirovali gigantskie impul'sy ot ocherednogo pul'sara. Primerno kazhdyi 270-i impul's v 40 raz prevoshodit po intensivnosti tipichnoe znachenie. Samyi sil'nyi iz obnaruzhennyh impul'sov prevoshodil srednii v 260 raz.


Vypusk 114. 08-29 avgusta 2005

astro-ph/0508206 Otkrytie bystryh rentgenovskih oscillyacii v gigantskoi vspyshke 1998 goda istochnika SGR 1900+14 (Discovery of Fast X-ray Oscillations During the 1998 Giant Flare from SGR 1900+14)
Authors: Tod E. Strohmayer, Anna L. Watts
Comments: 13 Pages, 5 figures, AASTeX, accepted for publication in the Astrophysical Journal Letters

Ochen' vazhnoe otkrytie, dopolnyayushee analogichnoe obnaruzhenie oscillyacii u drugogo istochnika myagkih povtoryayushihsya gamma-vspleskov SGR 1806-20 vo vremya dekabr'skoi vspyshki 2004 goda, sdelannoe Nandoi Rea (Nanda Rea) s kollegami.

V hvoste gigantskoi vspyshki obnaruzheny kvaziperiodicheskie kolebaniya s chastotoi 84 gerca. Eti kolebaniya svyazyvayut s torsionnymi kolebaniyami neitronnyh zvezd.

Oba rezul'tata (i po SGR 1806-20, i po SGR 1900+14) byli predmetami interesnyh diskussii na nedavnei konferencii po neitronnym zvezdam v Vankuvere.


astro-ph/0508534 Otkrytie radioizlucheniya ot tranzientnogo anomal'nogo rentgenovskogo pul'sara XTE J1810-197 (Discovery of Radio Emission from Transient Anomalous X-ray Pulsar XTE J1810-197)
Authors: J.P. Halpern et al.
Comments: 13 pages, 1 figure, to appear in ApJ Letters

Anomal'nyi rentgenovskii pul'sar XTE J1810-197 nablyudalsya v aktivnoi faze v 2003 g. V to vremya on byl otkryt kak bystro oslabevayushii ob'ekt s tipichnymi parametrami dlya istochnikov etogo klassa. Vse bylo obychnym, krome dostatochno bystro (mesyacy) ubyvayushei svetimosti. Arhivnye dannye pokazali nalichie slabogo ob'ekta na meste XTE J1810-197 (svetimost' poryadka na dva men'she, chem nablyudavshayasya v 2003 g.). Eto ne edinstvennyi tranzient sredi anomal'nyh rentgenovskih pul'sarov (ARP). Vtoroi ob'ekt s podobnymi svoistvami - AX J1844.8-0256.

Avtory dokladyvayut ob obnaruzhenii radioistochnika v napravlenii na XTE J1810-197. Istochnik ne pul'siruyushii. Priroda izlucheniya do konca ne yasna. Vozmozhno, chto veter chastic vysokoi energii obrazuet tumannost' vokrug ARP, kotoraya i proyavlyaet sebya v radio. Avtory obsuzhdayut vozmozhnost' nalichiya plotnoi sredy vokrug XTE J1810-197, chto i privodit k nablyudaemomu radioizlucheniyu.

Vtoroi tranzientnyi ARP AX J1844.8-0256 v radio zaregistrirovan ne byl. Odnako, veroyatno chto on nahoditsya dal'she, chem XTE J1810-197 (rasstoyaniya do ARP sil'no neopredelenny).

Vypusk 113. 01-08 avgusta 2005

astro-ph/0508050 Pul'sar s massoi 2.1 solnechnoi, izmerennoi po relyativistskomu sokrasheniyu orbity (A 2.1 Solar Mass Pulsar Measured by Relativistic Orbital Decay)
Authors: David J. Nice et al.
Comments: 9 pages, Submitted to ApJ

Kak izvestno, za schet izlucheniya gravitacionnyh voln orbity dvoinyh sistem sokrashayutsya (t.e. umen'shaetsya bol'shaya poluos'). Etot effekt horosho izmeren, naprimer, dlya dvuh dvoinyh radiopul'sarov. Takie izmereniya pozvolyayut poluchit' ochen' tochnuyu ocenku mass. Dlya dvuh dvoinyh pul'sarov massy sostavlyayut ot 1.2 do 1.4 mass Solnca.

Opredeleniya mass - vazhneishaya vesh' dlya izucheniya neitronnyh zvezd. Delo v tom, chto dannye po massam pozvolyayut ogranichivat' teorii vnutrennego stroeniya neitronnyh zvezd. I zdes' chrezvychaino vazhno nahodit' massivnye ob'ekty.

V stat'e predstavleny dannye po pul'saru, vhodyashemu v paru s belym karlikom. Dlya etoi sistemy obnaruzheno sokrashenie orbity. Otsyuda udalos' poluchit' ocenku massy neitronnoi zvezdy: 2.1 +/- 0.2 massy Solnca. Eto samaya bol'shaya na segodnyashnii den' massa neitronnoi zvezdy, izmerennaya stol' tochnym sposobom.


obzor astro-ph/0508056 Ohlazhdenie kompaktnyh zvezd (The Cooling of Compact Stars)
Authors: Dany Page, Ulrich Geppert, Fridolin Weber
Comments: Invited review for a special issue of Nucl. Phys. A. 44 pages, 18 figures

Bol'shoi podrobnyi obzor, posvyashennyi ohlazhdeniyu neitronnyh i kvarkovyh zvezd. Napomnyu, chto vazhnost' momenta v tom, chto nablyudeniya ostyvayushih neitronnyh zvezd dayut nam edva li ne edinstvennuyu vozmozhnost' uznat' hot' chto-to pro povedenie veshestva pri kolossal'nyh plotnostyah, prevoshodyashih yadernuyu.


Vypusk 112. 22-31 iyulya 2005

nucl-th/0507055 Poverhnost' strannyh zvezd (The Strange Star Surface: A Crust with Nuggets)
Authors: Prashanth Jaikumar, Sanjay Reddy, Andrew W. Steiner
Comments: 4 pages, 2 figures

Vozmozhno, chto strannye zvezdy eshe bolee neulovimy, chem eto schitalos' ranee. S 80-h godov bylo yasno, chto oni ochen' horosho maskiruyutsya pod obychnye neitronnye. Odnako nekotorye nadezhdy vozlagali na svoistva poverhnosti etih ob'ektov. Delo v tom, chto poverhnost' iz kvarkovogo veshestva budet nepohozhei na obychnuyu. V chastnosti, budut drugie mehanicheskie svoistva, drugaya teploprovodnost', i, glavnoe, k nei ne budet primenim eddingtonovskii predel svetimosti. V dannoi zhe rabote avtory stroyat model', v kotoroi poverhnost' kvarkovoi zvezdy (tochnee, ee kora) soderzhit kvarkovoe veshestvo v vide "samorodkov" (nuggets). V takom sluchae svoistva okazyvayutsya ochen' pohozhimi na svoistva obychnoi kory neitronnoi zvezdy. Esli eto i v samom dele tak, to vydelit' kvarkovye zvezdy budet eshe slozhnee. Pravda, ne dlya vseh tipov kvarkovyh zvezd takoe opisanie primenimo. Naprimer, dlya zvezd, veshestvo kotoryh nahoditsya v t.n. CFL (color flavor locked) faze, dannyi tip kory nevozmozhen.


Vypusk 111. 01-21 iyulya 2005

astro-ph/0507047 Vspyshka i kratkovremennoe uvelichenie pul'siruyushego potoka ot kandidata v magnitary 1E 1048.1-5937 (A Burst and Simultaneous Short-Term Pulsed Flux Enhancement from the Magnetar Candidate 1E 1048.1-5937)
Authors: Fotis P. Gavriil et al.
Comments: 24 pages, 4 figures, submitted to the Astrophysical Journal

Kak izvestno, kandidatami v magnitary yavlyayutsya dva tipa neitronnyh zvezd: istochniki myagkih povtoryayushihsya gamma-vspleskov (MPG) i anomal'nye rentgenovskie pul'sary (ARP). Pervye byli otkryty blagodarya svoei vspyshechnoi aktivnosti. Vtorye - blagodarya postoyannomu rentgenovskomu izlucheniyu. Odnako neskol'ko let nazad bylo pokazano, chto ARP mogut porozhdat' rentgenovskie vspyshki, vo mnogom podobnye vspleskam MPG. Ot istochnika 1E 1048.1-5937 (eto odin iz ARP) uzhe registrirovalis' vspyshki, i vot - eshe odna.

Primechatel'no, chto vspyshki ARP imeyut sushestvennoe otlichie ot slabyh (naibolee chasto vstrechayushihsya) vspyshek MPG. Eto - nalichie dlinnogo "hvosta", v kotorom i sosredotochena osnovnaya dolya vydelyaemoi energii. Vsplesk, kotoromu posvyashena dannaya zametka, osobenno vydelyaetsya. Posle osnovnoi vspyshki nablyudalsya rentgenovskii "hvost" dlitel'nost'yu okolo 700 sekund. Vozmozhno, pishut avtory, issledovanie etogo razlichiya pomozhet ponyat' raznicu mezhdu ARP i MPG.


astro-ph/0507052 Yarkostnoe ogranichenie na modeli ostyvaniya molodyh neitronnyh zvezd (Brightness constraint for cooling models of young neutron stars)
Authors: H. Grigorian
Comments: 12 pages 2 figures 1 table
astro-ph/0507061 Effekty sredy v ohlazhdenii neitronnyh zvezd i 3P2 neitronnaya shel' (Medium Effects in Cooling of Neutron Stars and $3P_2$ Neutron Gap)
Authors: H. Grigorian, D.N. Voskresensky
Comments: 18 p., 12 figs., widen version of astro-ph/0501678

Dve stat'i, posvyashennye raschetam ostyvaniya neitronnyh zvezd.

V pervoi rabote issleduetsya sistematika zavisimosti rezul'tatov raschetov v ramkah scenariya "nuclear meduim cooling" ot parametrov sverhtekuchesti i ot svoistv vneshnih sloev neitronnoi zvezdy. Takzhe vvoditsya "ogranichenie po yarkosti", sut' kotorogo sostoit v sleduyushem. Dlya neitronnyh zvezd s massoi primerno 1.1 massy solnca nedopustimy parametry, privodyashie k poyavleniyu bolee yarkih istochnikov, chem nablyudaemye v nastoyashii moment.

Vo vtoroi rabote provedeno detal'noe issledovanie zavisimosti rezul'tatov rascheta ot parametrov sheli sverhtekuchih neitronov.


astro-ph/0507206 Massa neitronnoi zvezdy v SMC X-1 (The mass of the neutron star in SMC X-1)
Authors: A.K.F. Val Baker, A.J. Norton, H. Quaintrell
Comments: Accepted for publication by A&A

Opredelenie mass neitronnyh zvezd - eto chrezvychaino vazhnaya, no, vmeste s tem, i chrezvychaino slozhnaya zadacha.

V ramkah nekotoryh model'nyh predpolozhenii avtory poluchayut verhnii predel na massu neitronnoi zvezdy v izvestnoi sisteme SMC X-1. Znachenie okazyvaetsya dostatochno nebol'shim: 1.21 +/- 0.1 massy Solnca. S drugoi storony standartnoe znachenie 1.4 lezhit vsego "v dvuh sigma".


astro-ph/0507420 Massa millisekundnogo pul'sara (The Mass of a Millisecond Pulsar)
Authors: B. A. Jacoby et al.
Comments: 12 pages, 3 figures, accepted for publication in ApJL

Vpervye dostatochno tochno izmerena massa millisekundnogo pul'sara. Ona okazalas' ravnoi 1.438 +/- 0.024 massy Solnca. Eto vazhnyi rezul'tat, t.k. mozhno ocenit' skol'ko veshestva neitronnaya zvezda uspela naakkrecirovat' poka raskruchivalas' vtorym komponentom sistemy. Eta velichina sostavlyaet menee 0.2 mass Solnca.


Vypusk 109. 01-14 iyunya 2005

astro-ph/0506280 Otkrytie gamma-izlucheniya ochen' vysokoi energii ot dvoinogo radiopul'sara PSR B1259-63 s pomosh'yu ustanovki H.E.S.S. (Discovery of the Binary Pulsar PSR B1259-63 in Very-High-Energy Gamma Rays around Periastron with H.E.S.S)
Authors: H.E.S.S. Collaboration: F. Aharonian
Comments: 10 pages, 8 figures, accepted in Astronomy and Astrophysics on 2 June 2005

Dvoinaya sistema PSR B1259-63/SS 2883 sostoit iz radiopul'sara i Ve-zvezdy. S pomosh'yu ustanovki H.E.S.S. udalos' obnaruzhit' zhestkoe gamma-izluchenie etoi sistemy.


Vypusk 108. 20-31 maya 2005

miniobzor astro-ph/0505491 Samye bol'shie magnitnye polya vo Vselennoi: anomal'nye rentgenovskie pul'sary i istochniki povtoryayushihsya gamma-vspleskov (The Highest Magnetic Fields in the Universe: Anomalous X-Ray Pulsars and Soft Gamma-ray Repeaters)
Authors: Sandro Mereghetti
Comments: To appear in the proceedings of the 40th Rencontres de Moriond "Very High Energy Phenomena in the Universe" - La Thuile, Italy (March 12-19, 2005) - 6 pages, 3 figures, 1 table

Ocherednoi obzor, posvyashennyi magnitaram i ih proyavleniyam, t.e. anomal'nym rentgenovskim pul'saram i istochnikam povtoryayushihsya gamma-vspleskov. Konechno zhe, chast' stat'i posvyashena dekabr'skoi vspyshke istochnika SGR 1806-20.


astro-ph/0505545 Gravitacionno-volnovaya astrometriya dlya bystrovrashayushihsya neitronnyh zvezd i opredelenie rasstoyanii do nih (Gravitational Wave Astrometry for Rapidly Rotating Neutron Stars and Estimation of Their Distances)
Authors: Naoki Seto
Comments: 6 pages, 1 figure, to appear in PRD

Avtor pokazyvaet, chto registraciya gravitacionnyh voln ot bystrovrashayushihsya neitronnyh zvezd mozhet pozvolit' poluchit' nezavisimuyu ocenku rasstoyaniya do nih s tochnost'yu poryadka 10 procentov.


obzor astro-ph/0505555 Pul'sary kak instrument dlya fundamental'noi fiziki i astrofiziki (Pulsars as Tools for Fundamental Physics and Astrophysics)
Authors: J. M. Cordes et al.
Comments: Chapter from "Science with the Square Kilometer Array" 26 pages, 6 figures; New Astronomy Reviews, 48, 2004, 1413

Proekt SKA smozhet otkryt' fakticheski vse pul'sary v Galaktike (tochnee, te, chto svetyat na nas). Eto otkroet novye vozmozhnosti ne tol'ko dlya izucheniya neitronnyh zvezd, no i novye vozmozhnosti dlya proverki ryada fundamental'nyh effektov. Svyazano eto, v pervuyu ochered', s tem, chto pul'sary - eto ochen' stabil'nye etalony vremeni. O tom, kakie zhe novye vozmozhnosti otkroyutsya pered uchenymi v otnositel'no nedalekom budushem, mozhno prochest' v obzore.


Vypusk 107. 11-19 maya 2005

astro-ph/0505191 INTEGRAL IGR J18135-1751=HESS J1813-178: novyi kosmicheskii uskoritel' vysokih energii ot keV do TeV (INTEGRAL IGR J18135-1751=HESS J1813-178: A new cosmic high energy accelerator from keV to TeV)
Authors: Ubertini et al.
Comments: Submitted to ApJ Letters; 12 pages, 3 Figures

V konce aprelya ya uzhe rasskazyval ob otkrytii novyh gamma istochnikov observatoriei HESS. Napomnyu, chto dlya dvuh iz nih ne bylo naideno sootvetstvuyushih ob'ektov v radio i rentgenovskom diapazone. Odnako Ubertini s kollegami smogli obnaruzhit' odin iz etih dvuh zagadochnyh istochnikov s pomosh'yu sputnika Integral.



Na vernem risunke pokazano izobrazhenie, poluchennoe INTEGRALOM. Interesuyushii nas istochnik sprava. Zelenym kruzhkom oboznachen istochnik HESS. Na nizhnem risunke pokazano radioizobrazhenie, poluchennoe na VLA v ramkah obzora neba. Krugi i ellipsy sootvetstvuyut oblastyam lokalizacii istochnika po dannym rentgenovskih sputnikov i HESS.

Priroda istochnika ostaetsya neizvestnoi. Avtory obsuzhdayut vozmozhnost' togo, chto eto pul'sarnaya tumannost' ili radiopul'sar v tesnoi dvoinoi sisteme.


astro-ph/0505255 Otkrytie bystryh rentgenovskih oscillyacii v hvoste gipervspyshki SGR 1806-20 (Discovery of Rapid X-ray Oscillations in the Tail of the SGR 1806-20 Hyperflare)
Authors: GianLuca Israel et al.
Comments: Accepted for publication on ApJ Letters. 4 Pages, 3 figures. emulateapj5 style used

Po dannym rentgenovskogo sputnika RXTE otkryty kvaziperiodicheskie kolebaniya v hvoste moshnoi vspyshki istochnika myagkih povtoryayushihsya vspleskov (MPG) SGR 1806-20. Eto pervoe otkrytie takogo roda. Vozmozhno, chto ono pomozhet prolit' svet na prirodu gigantskih vspyshek MPG.


Vypusk 106. 01-10 maya 2005

astro-ph/0505007 O vozmozhnosti togo, chto pary neitronnyh zvezd i chernyh dyr otvetstvenny za gamma-vspleski (On the viability of neutron star black hole binaries as central engines of gamma-ray bursts)
Authors: S. Rosswog
Comments: 8 pages, 2 Figures

Kak vy pomnite, gamma-vspleski delyatsya na korotkie (menee odnoi sekundy) i dlinnye (bolee 10 sekund) (sm. risunok po ssylke). Pervye ob'yasnyayutsya kak rezul'tat sliyaniya dvuh neitronnyh zvezd (i my nedavno rasskazyvali ob etom, eto byl kak raz obzor Stefana Rossvoga). Vtorye - akkreciei na chernuyu dyru posle vspyshki sverh(giper)novoi. Rezonno sprosit': a chto budet, esli slivaetsya neitronnaya zvezda i chernaya dyra? Ochevidno, chto neitronnaya zvezda budet razrushena, i vokrug chernoi dyry obrazuetsya disk. Situaciya kachestvenno pohozha na tu, chto schitaetsya prichinoi gamma-vspleska.

Stefan detal'no (naskol'ko eto seichas vozmozhno) issleduet sliyaniya neitronnyh zvezd i chernyh dyr. Ego rezul'taty govoryat o tom, chto svoistva obrazuyushihsya diskov ne pozvolyayut govorit' o generacii gamma-vspleskov.

Drugaya stat'ya na tu zhe temu (no uzhe bez detal'nyh chislennyh raschetov) predstavlena Coleman Miller'om. On takzhe podtverzhdaet, chto sliyaniya neitronnyh zvezd i chernyh dyr ne privodyat k poyavleniyu gamma-vspleska.


obzor astro-ph/0505073 Sverhtekuchest', dinamika i precessiya neitronnyh zvezd (Neutron Star Superfluidity, Dynamics and Precession)
Authors: M. Ali Alpar
Comments: 21 pages, one figure, to appear in the Proceedings of the NATO-ASI "The Electromagnetic Spectrum of Neutron Stars" held in Marmaris, Turkey, June 2004, eds. A. Baykal, S.K. Yerli, C. Inam and S. Grebenev

V pervuyu ochered' tekst posvyashen imenno precessii neitronnyh zvezd. Poskol'ku precessiya nablyudaetsya, my imeem vozmozhnost' poluchat' kosvennuyu informaciyu o vnutrennem stroenii neitronnyh zvezd po eshe odnomu kanalu.


Vypusk 105. 21-30 aprelya 2005

astro-ph/0504452 Aktivnost' gigantskih vspyshek magnitarov na ochen' bol'shih energiyah (Ultrahigh Energy Activity in Giant Magnetar Outbursts)
Authors: David Eichler
Comments: 11 pages

Tradicionno obychnye kosmicheskie gamma-vspleski rassmatrivayutsya kak vozmozhnye istochniki razlichnyh tipov chastic vysokih energii. Odnako vspyshka magnitara, proizoshedshaya 27 dekabrya, okazalas' sushestvenno yarche izvestnyh gamma-vspleskov (yarche s tochki zreniya zemnogo nablyudatelya, ee sobstvennoe energovydelenie, konechno zhe, ustupaet obychnym gamma-vspleskam). V svyazi s etim avtor rassmatrivaet gigantskie vspyshki magnitarov kak vozmozhnye istochniki kosmicheskih luchei sverhvysokih energii.

Otmetim, chto vyskazyvalis' mneniya o tom, chto kosmicheskie luchi sverhvysokih energii korreliruyut s ul'tramoshnymi IK galaktikami (sm., naprimer dve raboty Marii Giller i ee soavtorov astro-ph/0308532; astro-ph/0203337. Odnako vyvody o korrelyacii osparivalis', sm. astro-ph/0410741). V nashei stat'e s Borisom Shternom my obsuzhdali vozmozhnuyu svyaz' magnitarov s takimi galaktikami (sm. takzhe astro-ph/0502391). V nih chislo magnitarov dolzhno byt' bol'she. Ocenki pokazyvayut, chto temp gigantskih vspyshek mozhet sostavlyat' bolee odnoi vspyshki v god! Znachit, tam vyshe i veroyatnost' vstretit' molodoi magnitar. Takie istochniki mogut davat' ili bolee moshnye vspyshki (iz-za bOl'shego magnitnogo polya i men'shih periodov vrasheniya), ili zhe prosto vspyshki mogut idti chashe (tak, naprimer, glitchi radiopul'sarov chashe proishodyat u molodyh neitronnyh zvezd, gigantskie vspyshki mogut byt' svyazany s glitchami, t.o. estestvenno predpolozhit' rost ih chisla s umen'sheniem vozrasta neitronnoi zvezdy). V svete stat'i Davida Eihlera svyaz' kosmicheskih luchei sverhvysokih energii i galaktik s moshnym zvezdoobrazovaniem mozhet probresti novyi ottenok, svyazannyi s bOl'shim kolichestvom magnitarov (v tom chisle molodyh) v etih galaktikah.


miniobzor astro-ph/0504454 Magnitnye polya v zvezdnoi materii vysokoi plotnosti (Magnetic Fields in High-Density Stellar Matter)
Authors: German Lugones
Comments: Invited review, conference "Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures", Angra dos Reis, Brazil, Nov 28 - Dec 3, 2004, eds. E. M. de Gouveia dal Pino, G. Lugones & A. Lazarian, to be published in the AIP COnference Proceedings. 10 pages, no figures

Skvoz' prizmu teorii vnutrennego stroeniya neitronnyh zvezd (i voobshe, povedeniya veshestva pri sverhvysokih plotnostyah) daetsya obzor vliyaniya sil'nyh magnitnyh polei na astrofizicheskie proyavleniya neitronnyh zvezd.


astro-ph/0504479 Ogranicheniya na modeli populyacionnogo sinteza po populyacii dvoinyh neitronnyh zvezd (Constraining population synthesis models via the binary neutron star population)
Authors: R. O'Shaughnessy et al.
Comments: Submitted to ApJ. Uses emulateapj.cls. 8 pages + 7 figures

Kak izvestno, sliyaniya dvuh neitronnyh zvezd rassmatrivayutsya kak naibolee veroyatnye istochniki gravitacionnyh voln, kotorye smogut registrirovat' detektory tipa LIGO i VIRGO. Menee izvestno, chto raschety metodom populyacionnogo sinteza pokazyvayut, chto sliyaniya neitronnyh zvezd s chernymi dyrami mogut okazat'sya bolee veroyatnymi istochnikami (takim raschety provodilis', naprimer, v otdele Relyativistskoi astrofiziki GAISh pod rukovodstvom V.M. Lipunova). Odnako velika neopredelennost' v raschetah. Avtory predalagayut ispol'zovat' dannye po izvestnym sistemam, sostoyashim iz dvuh neitronnyh zvezd, dlya umen'sheniya etoi neopredelennosti. Eto lish' pervaya rabota avtorov v dannom napravlenii, tak chto "mnogoe sdelano, no mnogoe eshe predstoit".


astro-ph/0504584 Statisticheskoe issledovanie sobstvennyh dvizhenii 233 pul'sarov (A statistical study of 233 pulsar proper motions)
Authors: G. Hobbs, D. R. Lorimer, A. G. Lyne, M. Kramer
Comments: 20 pages, accepted by MNRAS

Ochen' vazhnaya rabota dlya vseh, kto zanimaetsya neitronnymi zvezdami.

Odnim iz vazhnyh parametrov neitronnoi zvezdy yavlyaetsya ee skorost' v moment rozhdeniya. Delo v tom, chto vo vremya vzryva sverhnovoi (ili srazu posle nego) znachitel'naya energiya mozhet byt' vydelena asimmetrichno, chto privedet k tomu, chto novorozhdennyi kompaktnyi ob'ekt poluchit tolchok (ego nazyvayut kik - kick). Udar mozhet byt' ochen' chuvstvitel'nym - neitronnaya zvezda mozhet razognat'sya do tysyach km/s! Vysokaya nachal'naya skorost' mozhet predopredelit' opredelennyi evolyucionnyi put' neitronnoi zvezdy v budushem. Naprimer, esli ona rodilas' v dvoinoi sisteme, to sistema mozhet byt' razrushena. Poetomu opredelenie raspredeleniya neitronnyh zvezd po skorostyam yavlyaetsya vazhneishei zadachei.

Naibol'shaya populyaciya neitronnyh zvezd - radiopul'sary. Mozhno nablyudat' ih sobstvennoe dvizhenie (na nebesnoi ploskosti). Togda, esli izvestno rasstoyanie, to mozhno opredelit' skorost' zvezdy v nebesnoi ploskosti. Dalee, esli schitat', chto skorosti raspredeleny sluchaino, mozhno poluchit' i ocenku istinoi (trehmernoi) skorosti. Takie raboty vedutsya s 70-h gg. Do poyavleniya dannoi stat'i naibolee obsheprinyatym raspredeleniem nachal'nyh skorostei neitronnyh zvezd schitalos' poluchennoe Arzumanyanom, Chernovym i Kordessom v 2002 g. Eto raspredelenie obladalo vazhnoi osobennost'yu - avtory obnaruzhili dve komponenty (dve mody). Srednyaya skorost' v pervoi mode - okolo 100 km/s, vo vtoroi - okolo 700 km/s. Poyavilos' mnozhestvo rabot, v kotoryh raznye avtory pytalis' ob'yasnit' etu bimodal'nost'. I vot ....

I vot avtory dannoi stat'i na osnovanii issledovaniya sobstvennyh dvizhenii 233 radiopul'sarov otvergayut bimodal'nost'!

Srazu skazhem, rezul'tat nuzhdaetsya v proverke. Eto ne iz nedoveriya k avtoram. Prosto pereschet nablyudaemogo raspredeleniya skorostei na nachal'noe raspredelenie yavlyaetsya ochen' slozhnoi zadachei s mnozhestvom neizvestnyh parametrov. Poetomu predpolozhim, chto stat'ya vyzovet diskussiyu. Te zhe samye vhodnye dannye budut ispol'zovany neskol'kimi gruppami dlya polucheniya nachal'nogo raspredeleniya po skorostyam.


Vypusk 103. 01-10 aprelya 2005

astro-ph/0504019 Otkrytie 10 pul'sarov v skaniruyushem obzore Aresibo (Discovery of 10 pulsars in an Arecibo drift-scan survey)
Authors: D.R. Lorimer et al.
Comments: 8 pages, 3 figures, accepted for publication in MNRAS

Na teleskope v Aresibo proveden ocherednoi poisk pul'sarov. Osmotr 1147 kvadratnyh gradusov privel k registracii 33 pul'sarov, iz kotoryh 10 - novye. Sredi novyh avtory vydelyayut eshe odin dvoinoi millisekundnyi pul'sar s malomassivnym kompan'onom. Oni polagayut, chto etot ob'ekt blagodarya shirokoi orbite i malomu ekscentrisitetu voidet v chislo pul'sarnyh par, ispol'zuyushihsya dlya proverki OTO.


astro-ph/0504075 Skirmionnye zvezdy: astrofizicheskaya motivaciya i prilozheniya (Skyrmion Stars: Astrophysical motivations and implications)
Authors: Prashanth Jaikumar, Rachid Ouyed
Comments: 10 pages and 7 figures

Skirmionnye zvezdy (Skyrmion stars aka SkyS) - eto po suti neitronnye zvezdy s ochen' interesnym uravneniem sostoyaniya, kotoroe dopuskaet sushestvovanie massivnyh ob'ektov (vplot' do 3.45 mass Solnca pri ochen' bystrom vrashenii). Nekotorye dannye izmerenii mass neitronnyh zvezd v tesnyh dvoinyh sistemah dayut dovol'no vysokie znacheniya: >2 mass Solnca. Poetomu uravneniya sostoyaniya, dlya kotoryh sushestvovanie takih ob'ektov vozmozhno, predstavlyayut bol'shoi interes.


miniobzor astro-ph/0504077 Magnitary (Magnetars)
Authors: Jeremy S. Heyl
Comments: 12 pages, 5 figures, XXII Texas Symposium on Relatistic Astrophysics

Podrobnyi obzor, posvyashennym magnitaram - sil'nozamagnichennym neitronnym zvezdam, ch'ya energetika svyazana s magnitnym polem (a ne s vrasheniem, ostyvaniem ili akkreciei).

My zhe v svoyu ochered' gotovim stat'yu o magnitarah i gigantskih vspyshshkah istochnikov myagkih povtoryayushihsya gamma-vspleskov dlya zhurnala Zemlya i Vselennaya. S predvaritel'nym variantom stat'i mozhno poznakomit'sya zdes'. Krome togo, lekciya ob etih ob'ektah budet prochitana na astrofeste.


Vypusk 102. 21-31 marta 2005

astro-ph/0503424 Otkrytie 105-millisekundnogo rentgenovskogo pul'sara v Kesteven 79 (Discovery of a 105 ms X-ray Pulsar in Kesteven 79: On the Nature of Compact Central Objects in Supernova Remnants)
Authors: E. V. Gotthelf et al.
Comments: 8 pages, 4 Figues. Latex, emulateapj.sty. To appear in the Astrophysical Journal

U central'nogo kompaktnogo istochnika v ostatke sverhnovoi Kes 79 obnaruzhen period 105 millisekund. Period byl zamechen po rentgenovskim nablyudeniyam na sputnike XMM-Newton.

Napomnim, chto v poslednie gody radiopul'sary poteryali svoi status "polnomochnyh predstavitelei" molodyh neitronnyh zvezd. Yasno, chto lish' nekotoraya (hotya i znachitel'naya) chast' molodyh neitronnyh zvezd proyavlyaet sebya kak obychnye radiopul'sary. Drugie vyglyadyat sovsem po-drugomu. Mozhno upomyanut' istochniki myagkih povtoryayushihsya gamma-vspleskov, anomal'nye rentgenovskie pul'sary, Velikolepnuyu semerku, kompaktnye istochniki v ostatkah sverhnovyh. K poslednemu klassu kak raz i otnositsya geroi rassmatrivaemoi stat'i.

V radiodiapazone etot pul'sar ne nablyudaetsya. Bolee togo, otsutstvuet dazhe pul'sarnaya tumannost', t.e. nel'zya skazat', chto aktivnyi pul'sar est', prosto ego luch ne popadaet na nas. Po vsei vidimosti pul'sar rodilsya s periodom, blizkim k nablyudaemomu, i s ne ochen' bol'shim magnitnym polem (po krainei mere <3 1012 Gs).


astro-ph/0503526 Novye issledovaniya pul'sarnoi tumannosti v ostatke sverhnovoi CTB 80 (New Studies of the Pulsar Wind Nebula in the Supernova Remnant CTB 80)
Authors: T.A. Lozinskaya et al.
Comments: to appear in Astronomy Letters, 12 pages, 6 postscript figures, two in colour; for a version with high resolution figures see http://www.sao.ru/hq/grb/team/vkom/CTB80_fine.pdf

Vpervye po issledovaniyu pul'sarnoi tumannosti udalos' opredelit' skorost' pul'sara vdol' lucha zreniya. Ona okazalas' dovol'no bol'shoi - okolo 500 km/s, chto prevoshodit ego skorost' v ploskosti nebesnoi sfery.


obzor physics/0503245 Neitronnye zvezdy (Neutron Stars)
Authors: Gordon Baym, Frederick K. Lamb
Comments: Encyclopedia of Physics 3rd ed., R.G. Lerner and G.L. Trigg, eds., Wiley-VCH, Berlin

Enciklopedicheskaya stat'ya o neitronnyh zvezdah. Rekomenduetsya vsem k obyazatel'nomu prochteniyu.


Zakanchivaetsya konkurs
Zvezdy AstroRuneta
Esli vy odin iz pyatisot ekspertov Astrotopa, no eshe ne golosovali v nominacii "Luchshii personal'nyi proekt", to vy mozhete prinyat' uchastie v sopernichestve saitov "Galaktika" i "Astrogalaktika" s nashimi "Obzorami astro-ph" i "ANKoi" !!!
Vash golos mozhet stat' reshayushim !!!!
Obratite vnimanie i na drugie nominacii, gde vy eshe ne progolosovali, a mogli by (v neskol'kih mogut golosovat' i ne-eksperty).


Vypusk 101. 11-20 marta 2005

astro-ph/0503239 Otkrytie pul'sacii i spektral'noi detali v rentgenovskom izluchenii odinochnoi neitronnoi zvezdy 1RXS J214303.7+065419/RBS 1774 (Detection of pulsations and a spectral feature in the X-ray emission of the isolated neutron star 1RXS J214303.7+065419/RBS 1774)
Authors: S. Zane et al.
Comments: 21 pages, 5 figures, ApJ accepted

Opredelen period dlya eshe odnogo ob'ekta iz Velikolepnoi semerki. Eto istochnik 1RXS J214303.7+065419/RBS 1774. Period okazalsya pohozhim na drugie izvestnye dlya neitronnyh zvezd etogo tipa -- 9.437 sekundy. Krome togo, v spektre obnaruzhena nekotoraya osobennost', no ee priroda poka ostaetsya neizvestnoi.


astro-ph/0503287 Gravitacionnoe izluchenie akkreciruyushego millisekundnogo pul'sara s magnitnouderzhivaemoi goroi (Gravitational Radiation from an Accreting Millisecond Pulsar with a Magnetically Confined Mountain)
Authors: A. Melatos, D. J. B. Payne
Comments: 19 pages, 4 figures, accepted for publication in The Astrophysical Journal

V kachestve istochnika gravitacionnyh voln rassmotrena neitronnaya zvezda "v interesnom polozhenii".

Pri moshnoi akkrecii na neitronnye zvezdy veshestvo sushestvenno izmenyaet strukturu magnitnogo polya. Pole "zaryvaetsya" za schet vypavshego veshestva. Formiruetsya nekotoryi "poyas" na magnitnom ekvatore (veshestvo vypadaet v osnovnom na magnitnye polyusa). V svoyu ochered' magnitnoe pole prepyatstvuet proniknoveniyu chasti veshestva v oblast' magnitnogo ekvatora. T.o. obrazuetsya kucha (gora) veshestva. T.k. magnitnye polyusa vovse ne obyazany sovpadat' s "geograficheskimi" polyusami (t.e. magnitnaya os' ne sovpadaet s os'yu vrasheniya), to zvezda priobretaet kvadrupol'nyi moment, a, sledovatel'no, budet izluchat' gravitacionnye volny.

S odnoi storony, avtory pokazyvayut, chto ih bolee sovershenanya ocenka daet amplitudu gravitacionnyh voln vyshe, chem predskazyvalos' ranee. S drugoi storony, velichina vse ravno slishkom mala, chtoby mozhno bylo rasschityvat' na registraciyu sovremennymi versiyami LIGO i VIRGO.


astro-ph/0503386 Proverka obshei teorii otnositel'nosti po dvoinomu radiopul'saru: svezhie rezul'taty (Testing GR with the Double Pulsar: Recent Results)
Authors: M.Kramer et al.
Comments: Contribution to The 22nd Texas Symposium on Relativistic Astrophysics, Stanford University, December 2004, 7 pages, 2 figures

Kak horosho izvestno, otkrytie dvoinogo radiopul'sara s ochen' tesnoi orbitoi otkrylo novye perspektivy v proverke teorii otnositel'nosti. Dlya etogo nado na protyazhenii vozmozhno bolee dolgogo perioda vremeni nakaplivat' dannye po taimingu pul'sarov. Chto i delaetsya.

V stat'e v dostatochno populyarnoi forme opisany testy Obshei teorii otnositel'nosti, vozmozhnye v takih sistemah.


Vypusk 100. 01-10 marta 2005

astro-ph/0503030 Gamma nablyudeniya gigantskoi vspyshki magnitara SGR 1806-20 (Gamma-Ray Observations of a Giant Flare from The Magnetar SGR 1806-20)
Authors: D. M. Palmer et al.
Comments: Submitted to Nature 2005-02-02, revised 2005-03-01. 21 pp, incl. 6 figures

Predstavleny rezul'taty nablyudenii na sputnike Swift. Nichego principial'no novogo v sravnenii s drugimi rabotami zdes' ne dobavleno. Vazhno, chto dannye raznyh eksperimentov sovpadayut.


Vspyshka po dannym Swift

V pyatnicu 11 chisla v GAISh budet nebol'shoi doklad, posvyashennoi vspyshke SGR 1806-20. Prezentaciya v formate PowerPoint budet dostupna zdes'


astro-ph/0503046 Modelirovanie populyacii odinochnyh neitronnyh zvezd, evolyucioniruyushih s izlucheniem gravitacionnyh voln (Simulation of a population of isolated neutron stars evolving through the emission of gravitational waves)
Authors: C. Palomba
Comments: 31 pages, 17 figures; accepted in MNRAS

Eshe odin primer interesnogo populyacionnogo sinteza odinochnyh neitronnyh zvezd.

Esli neitronnye zvezdy obladayut elliptichnost'yu, to oni budut istochnikami gravitacionnyh voln. Bolee togo, esli sushestvuet podklass neitronnyh zvezd s malen'kim magnitnym polem i zametnoi asimmetriei formy, to ih evolyuciya budet opredelyat'sya izlucheniem gravvoln. Imenno takim ob'ektam i posvyashena stat'ya.

Podcherknem, sushestvovanie takogo podklassa kompaktnyh ob'ektov yavlyaetsya gipotezoi. Po vsei vidimosti vvod v stroi detektora gravitacionnyh voln VIRGO pozvolit ili otkryt' ih, ili nalozhit' sushestvennye ogranicheniya na ih kolichestvo ili parametry.


miniobzor astro-ph/0503047 Magnitnye polya neitronnyh zvezd: teoreticheskii obzor (Magnetic fields in neutron stars: A theoretical perspective)
Authors: Andreas Reisenegger et al.
Comments: Invited review, conference "Magnetic Fields in the Universe: from Laboratory and Stars to Primordial Structures", Angra dos Reis, Brazil, Nov 28 - Dec 3, 2004, eds. E. M. de Gouveia dal Pino, A. Lazarian, & G. Lugones, to be published in the AIP COnference Proceedings. 11 pages, no figures

Nebol'shoi obzor, posvyashennyi proishozhdeniyu i evolyucii magnitnogo polya neitronnyh zvezd.


astro-ph/0503171 Ogranicheniya na rasstoyanie do SGR 1806-20 po poglosheniyu neitral'nym vodorodom (Constraints on the distance to SGR 1806-20 from HI absorption)
Authors: N. M. McClure-Griffiths, B. M. Gaensler
Comments: 3 pages, 1 embedded EPS figure, uses emulateapj.sty

V nedavnei stat'e Kamerona s soavtorami byla vyskazana tochka zreniya, chto rasstoyanie do vspyhnuvshego v dekabre MPG sostavlyaet ne 15 kpk, kak eto prinyato schitat', a ot 6 do 9 kpk. Konechno, takoe ponizhenie rasstoyaniya ne menyaet nichego principial'no, tem ne menee vazhno razobrat'sya.

V dannoi stat'e avtory rassmatrivayut ogranichenie na rasstoyanie do SGR 1806-20 po poglosheniyu v neitral'nom vodorode. Oni podtverzhdayut nizhnii predel, predlozhennyi Kameronom s soavtorami. Odnako s verhnim predelom oni ne soglasny. T.o. prezhnyaya ocenka v 15 kpk v principe vse eshe "v igre".


Vypusk 99. 15-28 fevralya 2005

astro-ph/0502297 Gamma-vspleski ot kvarkovyh zvezd (Gamma-Ray Bursts from quark stars)
Authors: B. Paczynski, P. Haensel
Comments: 4 pages, submitted to MNRAS (Letters)

Prevrashenie neitronnoi zvezdy v kvarkovuyu soprovozhdaetsya vydeleniem kolossal'noi energii, sravnimoi tol'ko so vzryvom sverhnovoi ili so sliyaniem dvuh kompaktnyh ob'ektov. Poetomu uzhe dostatochno davno obsuzhdaetsya vozmozhnaya svyaz' gamma-vspleskov s kvarkovymi zvezdami. Chto zhe novogo predlagayut avtory obsuzhdaemoi stat'i?

Novizna svyazana vot s chem. Poyavlyayutsya ukazaniya na to, chto sredi obychnyh (dlinnyh) gamma-vspleskov pryachutsya dva raznyh tipa sobytii. Odin tip svyazan s bolee slabymi vspleskami, proishodyashimi bez obrazovaniya ul'tra-relyativistskih dzhetov. Vtoroi - soprovozhdaetsya poyavleniem takih obrazovanii. Oba svyazany so sverhnovymi tipa Ic, a raznica mozhet ob'yasnyat'sya tem, chto posle vzryva formiruyutsya raznye tipy kompaktnyh ob'ektov. Avtory polagayut, chto vtoroi tip vspleskov svyazan s tem, chto posle vzryva sverhnovoi i obrazovaniya protoneitronnoi zvezdy proishodit formirovanie kvarkovogo ob'ekta. Osnovnoe preimushestvo oni vidyat ne v dopolnitel'noi energetike, a v tom, chto poyavlenie poverhnosti kvarkovoi zvezdy mozhet privesti k tomu, chto vo vneshnee prostranstvo vyletyat tol'ko elektrony, pozitrony, neitrino, fotony, no nikak ne bariony! T.e. poverhnost' budet rabotat' kak svoeobraznaya membrana.

Avtory polagayut, chto rabotayushii seichas na orbite sputnik Swift smozhet dat' reshayushuyu informaciyu dlya podtverzhdeniya sushestvovaniya dvuh tipov klassicheskih gamma-vspleskov. Krome togo, hotya napryamuyu vryad li udastsya prodemonstrirovat' obrazovanie kvarkovoi zvezdy, tem ne menee mozhno nadeyat'sya na to, chto novaya informaciya proyasnit chto-to i v etom voprose.


astro-ph/0502329 Gigantskaya vspyshka ot SGR1806-20 s prilozheniem k korotkim gamma-vspleskam (A tremendous flare from SGR1806-20 with implications for short-duration gamma-ray bursts)
Authors: Hurley et al.
Comments: 27 pages, 5 figures. Submitted to Nature

27 dekabrya byla zaregistrirovana samaya moshnaya vspyshka ot istochnika povtoryayushihsya gamma-vspleskov. Za doli sekundy vydelilos' okolo 1046 ergov (Solnce izluchaet stol'ko za 10 000 let). Potok energii na Zemle sostavil okolo 1 erga na kvadratnyi santimetr.

Napomnim, chto istochniki myagkih povtoryayushihsya gamma-vspleskov (MPG) byli otkryty v 1979 godu, v pervuyu ochered' blagodarya otechestvennyh sputnikam Venera i Prognoz na priborah razrabotannoi gruppoi Mazeca.

Sovremennye teorii risuyut MPG kak sil'no zamagnichennye neitronnye zvezdy - magnitary. Perestroiki magnitnogo polya i privodyat k vspyshkam. Chetkoi odnoznachnoi modeli vspleskov poka net. O novyh teoriyah sm. svezhuyu zametku astro-ph/0502349.

Vspyshki byvayut treh osnovnyh vidov: slabye, promezhutochnye, gigantskie. Poslednyuyu vspyshku uzhe vydelili v otdel'nyh klass gipervspyshek.

V stat'e predstavleny osnovnye rezul'taty nablyudenii. Takzhe privedeny interesnye rassuzhdeniya, kasayushiesya vozmozhnoi svyazi takih vspyshek s podklassom zhestkih korotkih gamma-vspleskov. Delo v tom, cho sputnik tipa CGRO (pribor BATSE) mog by videt' takoi vsplesk s rasstoyaniya do 50 Mpk. Znachit, esli uzh v nashei Galaktike za 30 let nablyudenii my uvideli odnu takuyu vspyshku (kstati, rasstoyanie do MPG - 15 kpk), to iz ob'emy, ogranichennogo 50 Mpk BATSE mog by zaregistrirovat' 1-2 sotni takih yavlenii.

Zametim, chto razumno predpolozhit' sleduyushee, t.k. magnitary eto ochen' molodye i korotkozhivushie ob'ekty, to osnovnoi vklad v proizvodstvo takih gipervspyshek budut vnosit' galaktiki s vysokim tempom zvezdoobrazovaniya i vysokim tempom vspyshek sverhnovyh. Etomu posvyashena korotkaya zametka odnogo iz avtorov obzorov.

Privedem takzhe ssylki na ryad drugih svezhih rabot, poyavivshihsya v Arhive v svyazi s gigantskoi vspyshkoi magnitara.

Vsplesk byl zaregistrirovan neskol'kimi kosmicheskimi apparatami, v tom chisle i rossiiskim Koronas-F (detektor Gelikon), a takzhe rossiiskim priborom Konus na amerikanskom sputnike Wind. Apparatura Koronas-F smogla dazhe zafiksirovat' izluchenie vspyshki, otrazhennoe ot Luny. Eto pervyi podobnyi sluchai. Ob etom - v stat'e Mazeca i dr.

Rezul'taty moshnoi vspyshki byli obnaruzheny i v radiodiapazone. Ob etom mozhno prochest' v stat'yah astro-ph/0502393 i astro-ph/0502428.

Stat'ya astro-ph/0502428 interesna eshe i tem, chto avtory osparivayut tradicionnuyu ocenku rasstoyaniya do istochnika vspleska. Vmesto obychnyh 15 kpk oni predlagayut velichinu 6-10 kpk. Eto, razumeetsya, privodit k izmeneniyu ocenki energetiki vspleska, odnako, dazhe ee korrekciya v 3-5 raz v storonu umen'sheniya ostavlyaet vspyshku samoi moshnoi iz nablyudavshihsya ot MPG.

Rezul'taty rentgenovskih nablyudenii v period, predshestvovavshii vspyshke, summirovany v stat'e A XMM-Newton View of the Soft Gamma-ray Repeater SGR 1806--20: Long Term Variability in the pre-Super Giant Flare Epoch.

Poslednyaya iz poyavivshihsya v fevrale statei na temu vspyshki SGR 1806-20 posvyashena nablyudeniyam na pribore SPI na bortu sputnika Integral. Avtory v osnovnom rasskazyvayut o nablyudeniyah hvosta vspleska (napomnim, chto zhestkie gigantskie vspyshki soprovozhdayutsya "hvostom" bolee myagkogo pul'siruyushego izlucheniya, period pul'sacii raven periodu vrasheniya neitronnoi zvezdy). Svyazano eto s bol'shoi moshnost'yu vspleska: t.k. Integral obladaet priborami s ochen' bol'shoi sobirayushei ploshad'yu, to potok fotonov byl nastol'ko velik, chto na vremya osnovnogo pika sputnik prosto "oslep".

T.o. my priveli ssylki na vse osnovnye raboty po SGR 1806-20, opublikovannye v Arhive za poslednie dve nedeli.


hep-ph/0502166 Pul'sarnye kiki iz-za spin-1 cvetnoi sverhprovodimosti (Pulsar kicks via spin-1 color superconductivity)
Authors: Andreas Schmitt, Igor A. Shovkovy, Qun Wang
Comments: 4 pages, 2 figures

Proishozhdenie vysokih skorostei neitronnyh zvezd tak i ostaetsya zagadkoi. Predlozheny i predlagayutsya samye raznye mehanizmy. Kakie-to svyazany s dinamikoi vzryva sverhnovoi, kakie-to s magnitnymi polyami, a kakie-to so slozhnoi fizikoi v nedrah etih kompaktnyh ob'ektov. Novyi mehanizm, predlozhennyi v dannoi stat'e, otnositsya kak raz k poslednei gruppe. Bez detalei sut' svoditsya k vozmozhnoi anizotropii potoka neitrino iz yadra zvezdy za schet ekzoticheskoi fazy kvarkovogo veshestva. Interesnyi moment svyazan s tem, chto zvezda nabiraet skorost' postepenno 9po mere izlucheniya neitrino iz ostyvayushego yadra). Osnovnoi vklad v skorost' mozhet nabirat'sya na vremenah poryadka 10 000 let!

Vypusk 98. 01-14 fevralya 2005

miniobzor astro-ph/0502124 Galakticheskie skollapsirovavshie ob'ekty (Galactic Collapsed Objects)
Authors: Janusz Ziolkowski
Comments: 15 pages; presented at Vulcano Workshop 2004; to be published in "Frontier Objects in Astrophysics and Particle Physics", 2005

Horoshii nebol'shoi obzor, posvyashennyi neitronnym zvezdam i chernym dyram. Obo vsem po chut'-chut', no v itoge sobrano mnogo poleznyh dannyh po raznym tipam sistem s kompaktnymi ob'ektami. V osnovnom obsuzhdayutsya massy i magnitnye polya. Krome togo, rassmotreny sistemy s kvaziperiodicheskimi oscillyaciyami (QPO).


Vypusk 97. 17-31 yanvarya 2005

miniobzor astro-ph/0501357 Udarnye volny okolo pul'sarov i neitronnyh zvezd (Bow shocks around pulsars and neutron stars)
Authors: Bryan M. Gaensler
Comments: 12 pages, 2 embedded EPS figures, 1 GIF figure. Advances in Space Research, in press

V poslednie gody poyavlyaetsya vse bol'she danynh ob udarnyh volnah, voznikayushih vokrug neitronnyh zvezd. Dostatochno chasto poyavlenie volny svyazano s dvizheniem neitronnoi zvezdy v mezhzyvezdnoi srede. Okazyvaetsya, chto izuchenie takih golovnyh udarnyh voln mozhet rasskazat' mnogo novogo o samih neitronnyh zvezdah.


Vypusk 96. 01-16 yanvarya 2005

obzor astro-ph/0501226 Pul'sary v sharovyh skopleniyah (Pulsars in Globular Clusters)
Authors: Fernando Camilo, Frederic A. Rasio
Comments: Review included in proceedings of Aspen 2004 meeting "Binary Radio Pulsars"; 23 pages, 9 included EPS figures Journal-ref: ASP Conf. Ser. Vol. 328, 2005: Binary Radio Pulsars, eds. F. A. Rasio & I. H. Stairs (San Francisco: ASP), p. 147

Bolee 100 radiopul'sarov obnaruzheno v 24 sharovyh skopleniyah (napominim, chto samih skoplenii gorazdo bol'she, prosto ne vo vseh poka (?) obnaruzhili radiopul'sary). Fakticheski vse pul'sary millisekundnye, t.e. "raskruchennye" akkreciei. Eto starye neitronnye zvezdy, period vrasheniya kotoryh byl umen'shen za schet uglovogo momenta veshestva, natyanutogo s kompan'ona v tesnoi dvoinoi sisteme.

Pochti polovina izvestnyh radiopul'sarov v sharovyh skopleniyah nahoditsya v Terzan 5 i 47 Tukana. O skoplenii Terzan 5 est' otdel'naya svezhaya (dovol'no populyarnaya) stat'ya.


miniobzor astro-ph/0501264 Akkreciruyushie millisekundnye pul'sary (Accretion-driven millisecond X-ray pulsars)
Authors: Rudy Wijnands
Comments:To appear in Nova Science Publishers (NY) volume "Pulsars New Research"

Vyshe my napisali, chto millisekundnye radiopul'sary byli raskrucheny v tesnyh dvoinyh sistemah. Odnako dolgoe vremya astronomy ne mogli zaregistrirovat' akkreciruyushie millisekundnye pul'sary. Takie ob'ekty dolzhny byli by nablyudat'sya kak rentgenovskie istochniki. Lish' neskol'ko let nazad oni byli obnaruzheny.

Pervoi otkrytoi sistemoi etogo tipa stal istochnik SAX J1808.4-3658 (SAX v nazvanii ukazyvaet, chto otkrytie bylo sdelano na sputnike BeppoSAX). Imenno etomu ob'ektu posvyashena bOl'shaya chast' predstavlyaemogo obzora.

Otmetim zdes' i druguyu svezhuyu stat'yu. "Constraining Brans-Dicke Gravity with Millisecond Pulsars in Ultracompact Binaries". V nei predlagaetsya ispol'zovat' pyat' izvestnyh akkreciruyushih millisekundnyh rentgenovskih pul'sarov dlya proverki teorii gravitacii.


Vypusk 95. 22-31 dekabrya 2004

miniobzor astro-ph/0412278 Fizika pul'sarov na nizkih chastotah (Pulsar Physics at Low Frequencies)
Authors: J. A. Eilek et al.
Comments: 7 pages

Empiricheskaya "standartnaya model'" radiopul'sarov dostatochno ploho opisyvaet ih svoistva, nablyudayushiesya na samyh nizkih radiochastotah (desyatki i sotni megagerc). Chem eto mozhno ob'yasnit' i kak etu model' skorrektirovat' osnovnye voprosy, rassmatrivaemy v dannoi publikacii.


astro-ph/0412327 Obrazovanie massivnyh skirmionnyh zvezd (Formation of massive skyrmion stars)
Authors: S.B.Popov , M.E.Prokhorov
Comments: 8 pages, 3 figures, submitted to A&A

A eto nasha stat'ya (avtorov obzorov).

Skirmionnye zvezdy eto neitronnye zvezdy s ochen' zhestkim uravneniem sostoyaniya. Samo uravnenie sostoyaniya bylo predlozheno v 1999 g. Ouedom i Batlerom, a model', na osnove kotoroi kravnenie postroeno byla sozdana Skirmom v 1962 godu. Seichas k etomu uravneniyu sostoyaniya snova voznik interes. Delo v tom, chto dazhe bez vrasheniya massa takoi zvezdy mozhet dostigat' pochti 3 Solnechnyh, a na predele vrasheniya do 3.45 mass Solnca. Takie ekstremal'nye parametry dolzhny pozvolit' dostatochno legko oprovergnut' ili podtverdit' dannoe uravnenie sostoyaniya. Nuzhno tol'ko ponyat' v kakim sistemah poyavlenie stol' massivnyh neitronnyh zvezd naibolee veroyatno.

My nashli semeistvo evolyucionnyh trekov dvoinyh sistem, v kotoryh neitronnaya zvezda za schet akkrecii uvelichivaet svoyu massu ot standartnoi velichiny (1.4 massy Solnca) do ochen' vysokih znachenii (2-3 massy Solnca).

Takih zvezd v Galaktike dolzhno byt' neskol'ko desyatkov tysyach. Oni mogut proyavlyat' sebya kak millisekundnye pul'sary (radio ili rentgenovskie) ili kak nepul'siruyushie rentgenovskie istochniki, v kotoryh akkrecionnyh disk dohodit neposredstvenno do poverhnosti neitronnoi zvezdy.


katalog astro-ph/0412641 Katalog pul'sarov ATNF (The ATNF Pulsar Catalogue)
Authors: R N Manchester, G B Hobbs, A Teoh & M Hobbs
Comments: 29 pages, 4 figs. Accepted by Astron. J

Poyavilas' stat'ya-opisanie superkataloga radiopul'sarov. Pol'zovat'sya im ochen' udobno. Dlya specialistov po radiopul'saram - eto instrument nomer odin.


astro-ph/0412662 O polyarnyh shapkah "Treh Mushketerov" (On the polar caps of the 3 Musketeers)
Authors: A. De Luca et al.
Comments: 42 pages, 17 figures, accepted in ApJ

Odinochnye neitronnye zvezdy PSR B0656+14, PSR B1055-52 i Geminga byli nazvany "Tremya Mushketerami" Bekerom i Tryumperom v 1997 godu. Nablyudeniya etoi troiki s borta XMM-Newton nastol'ko uvelichili kolichestvo zaregistrirovannyh kvantov, chto pozvolili poluchit' ih vysokotochnuyu sinhronnuyu (privyazannuyu k faze osevogo vrasheniya neitronnoi zvezdy) rentgenovskuyu spektroskopiyu. Spektry etih ob'ektov horosho opisyvayutsya trehkomponentnoi model'yu. Pervye dva komponenta yavlyayutsya teplovymi: pervyi - bolee holodnyi - po vidimomu ispuskaetsya vsei poverhnost'yu neitronnoi zvezdy. Istochnikom vtorogo, bolee goryachego, yavlyayutsya goryachie tochki - shapki na magnitnyh polyusah. Razmery shapok u etih treh pul'sarov sil'no razlichayutsya. I tretii stepennoi neteplovoi komponent, intensivnost' kotorogo menyaetsya sinhronno s fazoi vrasheniya. Ostal'nye podrobnosti (i grafiki spektrov) v stat'e.


Vypusk 94. 13-21 dekabrya 2004

astro-ph/0412404 Podhod, ob'yasnyayushii bol'shoe vremya ohlazhdeniya anomal'nyh rentgenovskih pul'sarov i istochnikov povtoryayushihsya gamma-vspleskov (An Approach to Explain the Long Cooling Times of Anomalous X-ray Pulsars and Soft Gamma Repeaters with the Neutrino Magnetic Moment)
Authors: Efe Yazgan, Mehmet T. Zeyrek
Comments: 6 pages, 1 figure
astro-ph/0412515 Izluchenie neitrino strannymi zvezdami s bol'shimi magnitnymi polyami (The Neutrino Emissivity of Strange Stars with Ultra Strong Magnetic Field)
Authors: Liu Xuewen, Zheng Xiaoping, Hou Defu
Comments: 10 pages, 2 figures

Dve stat'i, svyazannye obshei tematikoi: izluchenie neitrino sil'nozamagnichennymi neitronnymi zvezdami.

Avtory pervoi stat'i pytayutsya ob'yasnit', pochemu magnitary dolzhny byt' goryachimi. Oni polagayut, chto nalichie u neitrino nebol'shogo magnitnogo momenta privedet v dlinnym vremenam ohlazhdeniya sil'nozamagnichennyh zvezd. Vo vtoroi stat'e situaciya pryamo protivopolozhna: avtory pokazyvayut, chto strannye zvezdy s bol'shim magnitnym polem budut ostyvat' bystro. Konechno, osnovnye vyvody dvuh statei drug drugu ne protivorechat, no dlya ob'yasneniya prirody nablyudaemyh magnitarov (naprimer, v istochnikah povtoryayushihsya gamma-vspleskov i v anomal'nyh rentgenovskih pul'sarah) dolzhno podhodit' tol'ko chto-to odno (ili ni odnogo).


Vypusk 93. 01-12 dekabrya 2004

miniobzor astro-ph/0412215 Strannoe kvarkovoe veshestvo v zvezdah (Strange Quark Matter in Stars: A General Overview)
Authors: Jurgen Schaffner-Bielich
Comments: 8 pages, 1 figure, plenary talk given at the 8th International Conference on Strangeness in Quark Matter (SQM2004), Cape Town, South Africa, 15-20 September 2004

Korotkii obzor po kvarkovym zvezdam. Vklyucheno mnogo ssylok na novye raboty (kak teoreticheskie, tak i nablyudatel'nye). Stil' stat'i podrazumevaet, chto chitatel' znakom s tematikoi (neitronnye i kvarkovye zvezdy) hotya by na horoshem populyarnom urovne.


Vypusk 92. 15-30 noyabrya 2004

astro-ph/0411507 Dinamika pul'sarov: peresmotr modeli magnitnogo dipolya (Pulsar dynamics: magnetic dipole model revisite)
Authors: G. Lugones, I. Bombaci
Comments: 4 pages, 3 figures, submitted to Physical Review Letters

Na nash vzglyad - eto vazhnaya i interesnaya rabota. Odin iz voprosov, kotoryi my zadaem sebe - "pochemu my sami ne dogadalis'?" (odin iz avtorov napisal nam, chto on sam byl udivlen, chto za 37 let izucheniya pul'sarov nikto ne sdelal takih prostyh ocenok).

Avtory obrashayutsya k klassicheskoi modeli zamedleniya neitronnoi zvezdy. V etoi modeli vrashenie tormozitsya za schet sushestvovaniya magnitnogo polya. Ne smotrya na neprekrashayushiesya spory o detalyah processa tormozheniya, vse shodyatsya v tom, chto prostaya magnito-dipol'naya formula neploho opisyvaet deistvitel'nost'. Imenno takaya formula ispol'zuetsya dlya ocenki magnitnogo polya i vozrasta pul'sara po tempu ego zamedleniya.

German Lugones i Ignacio Bombachi rassmotreli, chto budet, esli prosteishim obrazom uchest' neodnorodnost' vrasheniya neitronnoi zvezdy. Poluchennye rezul'taty dostatochno interesny.
1. Magnitnoe pole okazyvaetsya raza v 4 vyshe, chem pole, opredelennoe po standartnoi formule. Eto dovol'no interesno, t.k. okolo 100 pul'sarov okazyvayutsya v oblasti sverhkriticheskogo (sverhshvingerovskogo) polya.
2. Vozrast pul'sara, ocenivaemyi po periodu i proizvodnoi perioda, okazyvaetsya sushestvenno zavisyashim ot nachal'nogo perioda. Eto mozhet pomoch' snyat' protivorechie v raznyh ocenkah vozrasta po parametram perioda i po nablyudaemym ostatkam sverhnovyh.


astro-ph/0411560 Grelka dlya stareyushih neitronnyh zvezd (A Hot Water Bottle for Aging Neutron Stars)
Authors: Mark Alford et al.
Comments: 14 pages, 5 figures

Kvantovaya hromodinamika predskazyvaet, chto pri vysokih plotnostyah, harakternyh dlya nedr neitronnyh zvezd, veshestvo mozhet okazyvat'sya v razlichnyh interesnyh sostoyaniyah. Detali eto izucheny kraine ploho, chto svyazano kak s trudnost'yu raschetov, tak i s otsutstviem eksperimental'nyh dannyh. Poetomu fiziki vse chashe i chashe obrashayutsya k astronomicheskim dannym.

V etoi stat'e avtory predskazyvayut, chto nalichie dazhe nebol'shogo kolichestva veshestva v odnoi iz takih interesnyh faz (my ne budem vdavat'sya v detali, chto takoe gapless color-flavour locked phase) privedet k tomu, chto ohlazhdenie zvezdy na fotonnoi stadii (kogda izluchenie neitrino uzhe ne vnosit osnovnogo vklada, a energiya unositsya fotonami s poverhnosti) poidet medlennee standartnogo. Kak budto v nedrah zvezdy est' grelka, kotoraya ne daet ei bystro ostyt'.

Nablyudeniya neitronnyh zvezd s vozrastami poryadka milliona let (eto mogut byt' ob'ekty Velikolepnoi semerki) dolzhny v budushem dat' otvet na vopros o neobhodimosti takoi grelki.

Sm. takzhe stat'yu po ostyvaniyu gibridnyh zvezd.


astro-ph/0411796 PSR J1756-2251: novaya relyativistskaya dvoinaya neitronnaya zvezda (PSR J1756-2251: a new relativistic double neutron star system)
Authors: A.J.Faulkner et al.
Comments: Accepted by ApJ Letters. 4 published pages, 3 figures and 2 tables

Po vsei vidimosti otkryta novaya sistema, sostoyashaya iz dvuh neitronnyh zvezd, odna iz kotoryh nablyudaetsya kak radiopul'sar. Nablyudeniya pokazali, chto polnaya massa sistemy PSR J1756-2251 sostavlyaet 2.574+/-0.003 solnechnoi massy (na samom dele, poka ocenka model'no zavisima). Odin iz komponent - pul'sar - tochno yavlyaetsya neitronnoi zvezdoi. Massy neitronnyh zvezd sostavlyayut 1.2-2 solnechnye massy. Znachit, na vtoroi kompan'on prihoditsya primerno 0.6-1.4 massy solnca. Veroyatnee vsego, on yavlyaetsya malomassivnoi neitronnoi zvezdoi s massoi <1.25 massy solnca.


Vypusk 91. 01-14 noyabrya 2004

astro-ph/0411103 Neitronnye zvezdy s kvarkovymi yadrami. II. Osnovnye integral'nye parametry i struktura (Neutron Stars with a Quark Core. II.Basic Integral and Structural parameters)
Authors: G.B.Alaverdyan, A.R.Harutyunyan, Yu.L.Vartanyan
Comments: 13 pages, 4 figures

My neodnokratno pisali o razlichnyh aspektah fiziki i astrofiziki kvarkovyh zvezd. Vot novaya rabota.

V Armenii tradicionno zanimalis' i zanimayutsya neitronnymi zvezdami (napomnim, chto pervaya stat'ya po kvarkovym zvezdam byla opublikovana imenno v armyanskom zhurnale Astrofizika, hotya i ne armyanskimi avtorami). V etoi rabote avtory stroyat konfiguracii neitronnyh zvezd s kvarkovymi yadrami i opisyvayut osnovnye parametry takih ob'ektov.

astro-ph/0411207 Izmereniya dvoinyh pul'sarov s belymi karlikami na Aresibo: Ukazaniya na nalichie tyazhelyh neitronnyh zvezd (Arecibo Measurements of Pulsar--White Dwarf Binaries: Evidence for Heavy Neutron Stars)
Authors: David J. Nice et al.
Comments: 2 pages, 1 figure, to appear in PASP conf series

Avtory sobrali dannye o massah neitronnyh zvezd, vhodyashih v pary s belymi karlikami, kotorye byli polucheny po izmereniyu ih taiminga na radioteleskope v Aresibo. Srednyaya massa neitronnyh zvezd v poluchennoi vyborke vyshe kanonicheskogo znacheniya 1.35Mo.


miniobzor astro-ph/0411243 Rentgenovskaya observatoriya Chandra: nablyudeniya neitronnyh zvezd (The Chandra X-Ray Observatory: Observations of Neutron Stars)
Authors: Martin C. Weisskopf
Comments: 12 pages, 8 figures, NATO ASI Proceedings

Naibolee izvestnaya osobennost' observatorii Chandra, rabotayushei v myagkoi rentgenovskoi oblasti spektra, umenie stroit' izobrazheniya, ne ustupayushie po razresheniyu opticheskim, poluchennym na nebol'shih nazemnyh teleskopah. Chandra nablyudaet vse: zvezdy, rentgenovskie istochniki, ostatki sverhnovyh, obychnye i aktivnye galaktiki, ih skopleniya, kvazary i t.d. Dannyi obzor posvyashen tol'ko neitronnym zvezdam.


obzor nucl-th/0410091 Dve lekcii po cvetnoi sverhprovodimosti (Two lectures on color superconductivity)
Authors: Igor A. Shovkovy
Comments: 56 pages, 9 figures. Minor corrections and references added. Lectures delivered at the IARD 2004 conference, Saas Fee, Switzerland, June 12 - 19, 2004, and at the Helmholtz International Summer School and Workshop on Hot points in Astrophysics and Cosmology, JINR, Dubna, Russia, August 2 - 13, 2004

Eto ne sovsem astrofizicheskie lekcii. Odnako takoe ekzoticheskoe yavlenie kak cvetnaya sverhprovodimost' (osnovannaya na sparivanii kvarkov, a ne elektronov ili protonov) mozhet sushestvovat' v nedrah kompaktnyh ob'ektov - kvarkovyh zvezd. Poetomu my sochli umestnym pomestit' etot otryvok v nashem obzore. Tem bolee, chto sami lekcii my slyshali, i schitaem, chto ih avtor sovershenno zasluzhenno byl priznan luchshim lektorom shkoly v Dubne!

A vot fotografiya iz Dubny, na kotoroi est' avtor lekcii i oba avtora obzorov (plyus neskol'ko drugih izvestnyh fizikov i astrofizikov).

nucl-th/0411016 Gibridnye zvezdy, maskiruyushiesya pod neitronnye (Hybrid stars that masquerade as neutron stars)
Authors: Mark Alford et al.
Comments:21 pages, LaTeX

Avtory pokazyvayut, chto gibridnye zvezdy, imeyushie kvarkovoe yadro i normal'nye vneshnie sloi, mogut imet' otnoshenie massy k radiusu primerno takoe zhe kak u obychnyh neitronnyh zvezd. Eto oznachaet, chto vydelit' takie ob'ekty budet oh kak neprosto!

Vypusk 90. 25-31 oktyabrya 2004

obzor astro-ph/0410536 Akkreciruyushie neitronnye zvezdy i chernye dyry: desyatiletie otkrytii (Accreting Neutron Stars and Black Holes: A Decade of Discoveries)
Authors: Dimitrios Psaltis (University of Arizona)
Comments: 42 pages; 24 figures. To appear in "Compact Stellar X-ray Sources", eds. W.H.G. Lewin and M. van der Klis

Glava iz knigi, posvyashennoi kompaktnym rentgenovskim istochnikam. Avtor daet podrobnyi obzor osnovnyh otkrytii (i nablyudatel'nyi i teoreticheskih) v oblasti issledovanii akkreciruyushih neitronnyh zvezd i chernyh dyr za poslednee desyatiletie.

Mnogo poleznyh tablic, a takzhe ogromnyi spisok ssylok na original'nye issledovaniya.


obzor astro-ph/0410551 Obzor bystroi peremennosti v rentgenovskih (A review of rapid X-ray variability in X-ray binaries)
Authors: M. van der Klis
Comments: 73 pages, 21 figures, no color to appear in Compact stellar X-ray sources, Lewin & van der Klis (eds), Cambridge University Press

Eshe odna glava iz "Compact stellar X-ray sources".

van der Klis yavlyaetsya, pozhalui, samym krupnym ekspertom po QPO - kvaziperiodicheskim oscillyaciyam, Etot tip peremennosti nablyudaetsya u akkreciruyushih neitronnyh zvezd i chernyh dyr. Po QPO mozhno poluchat' vazhnuyu informaciyu o parametrah sistem.


miniobzor astro-ph/0410607 Biografiya magnitnogo polya u neitronnyh zvezd (A Biography of the Magnetic Field of a Neutron Star)
Authors: Malvin Ruderman (Columbia University)
Comments: Latex 16 pages, 3 figures

Izvestnyi specialist po neitronnym zvezdam - Malvin Ruderman - daet nabrosok biografii neitronnoi zvezdy ot ee detstva do dovol'no "zrelogo" vozrasta. Osnovnoe vnimanie udelyaetsya evolyucii magnitnogo polya.

Posle korotkogo perioda ochen' intensivnogo ostyvaniya tol'ko chto rodivsheisya neitronnoi zvezdy my poluchaem vrashayushuyusya zamagnichennuyu kanonicheskuyu neitronnuyu zvezdu: so sverhprovodyashimi protonami, sverhtekuchimi neitronami i predel'no vyrozhdennymi relyativistskimi elektronami v yadre, prichem vse eto okruzheno vysokoprovodyashei koroi. Dal'neishaya evolyuciya podobnogo ob'ekta predskazyvaet izmenenie orientacii magnitnogo dipolya, anomal'no malyi polyarnyi kasp u millisekundnyh pul'sarov i periodicheskie sboi vrasheniya - "glitchi".

Otmetim, chto narisovannaya v stat'e kartina dostatochno kachestvennaya, i real'nost' mozhet okazat'sya kuda slozhnee.


Vypusk 89. 18-25 oktyabrya 2004

astro-ph/0410488 Massy, parallaks i relyativistskii taiming dvoinogo pul'sara PSR J1713+0747 (Masses, Parallax, and Relativistic Timing of the PSR J1713+0747 Binary System)
Authors: Eric M. Splaver et al.
Comments: 12 pages, Accepted by ApJ

Dvoinoi pul'sar PSR J1713+0747 sostoit iz neitronnoi zvezdy vokrug kotoroi s periodom 68 dnei obrashaetsya belyi karlik. 12 let nablyudenii pozvolili dovesti srednyuyu tochnost' izmereniya momentov prihoda impul'sov do 200 ns i ocenit' sleduyushie parametry sistemy:

MNS= 1.3+/-0.2Mo
MWD= 0.28+/-0.03Mo
&pi= 0.89+/-0.08 mas
D= 1.1+/-0.1 kpk

Esli skombinirovat' chisto nablyudatel'nuyu ocenku massy neitronnoi zvezdy s teoreticheskoi zavisimost'yu orbital'nyi period - massa yadra predsverhnovoi, to dlya neitronnoi zvezdy poluchitsya bolee vysokaya ocenka massy

MNS = 1.53+0.08-0.06Mo


Vypusk 87. 01-10 oktyabrya 2004

astro-ph/0410099 Spektral'nye i vremennyi harakteristiki v rentgenovskom diapazone dlya zvezd molodogo rasseyannogo skopleniya IC 2391 (X-ray spectral and timing characteristics of the stars in the young open cluster IC 2391)
Authors: A. Marino et al.
Comments: Astronomy & Astrophysics, in press

Na sputnike XMM-Newton provedeny nablyudeniya rasseyannogo skopleniya IC 2391. Proanalizirovany dannye po 99 individual'nym ob'ektam (zvezdam), iz nih 24 prinadlezhat skopleniyu.

Ostanovimsya tol'ko na odnom vyvode raboty. Sravnenie novyh dannyh s rezul'tatami staryh rentgenovskih nablyudenii na sputnike ROSAT pokazalo, chto u issledovannyh zvezd net ciklicheskih variacii svetimosti na masshtabe v 7 let (promezhutok vremeni mezhdu nablyudeniyami). T.e., delayut vyvod avtory, dolgoperiodicheskie variacii, podobnye solnechnomu 11-letnemu ciklu, ne yavlyayutsya tipichnoi harakteristikoi issledovannyh molodyh zvezd.


Vypusk 86. 20-30 sentyabrya 2004

astro-ph/0409651 Proishozhdenie dvoinogo pul'sara J0737-3039B (The Origin of the Binary Pulsar J0737-3039B)
Authors: Tsvi Piran, Nir J. Shaviv
Comments: 4 pages, 2 figures, submitted to PRL

Avtory rassmatrivayut dva evolyucionnyh scenariya, privodyashih k obrazovaniyu podobnoi sistemy. Soglasno pervomu iz nih molodoi radiopul'sar J0737-3039B obrazovalsya pri vzryve gelievoi zvezdy s massoi M>2.1-2.3Mo. V etom sluchae centr mass sistemy dvuh neitronnyh zvezd posle etogo (vtorogo v sisteme) vzryva sverhnovoi priobretet skorost' bolee 120 km/s, chto ploho soglasuetsya s malym udaleniem (~50 pk) sistemy ot ploskosti Galaktiki. Vo vtorom scenarii vzryvaetsya ochen' neobychnaya predsverhnovaya s massoi 1.45Mo (napomnim, chto massa J0737-3039B sostavlyaet 1.25Mo). Podobnye vzryvy eshe ne nablyudalis'. Vtoraya model' predskazyvaet men'shuyu prostranstvennuyu skorost' sistemy (60-70 km/s).

Dlya vybora mezhdu dvumya modelyami neobhodimo izmerit' sobstvennoe dvizhenie pul'sarov. Na segodnya ukazannye izmereniya byli provedeny na osnove mezhzvezdnyh pul'sacii i dali dva nesoglasuyushihsya rezul'tata: 141+/-9 km/s (bolee rannie izmereniya) i 66+/-15 km/s (novye izmereniya). Eti velichiny, kak mozhno videt', podhodyat libo k odnoi, libo k drugoi modeli.

Vyvod: neobhodimy bolee tochnye pryamye (radiointerferometricheskie) izmereniya sobstvennogo dvizheniya sistemy J0737-3039, chtoby vybrat' odnu iz dvuh modelei.


astro-ph/0409752 Massivnaya neitronnaya zvezda ili malomassivnaya chernaya dyra v istochnike 2S0921-630 (The massive neutron star or low-mass black hole in 2S0921-630)
Authors: T.Shahbaz et al.
Comments: 14 pages, 3 figures, 1 table, accepted by ApJ Lett.

V raspredelenii mass kompaktnyh ob'ektov v dvoinyh sistemah nablyudayutsya dva pika. Odin iz nih - neitronnye zvezdy. V sistemah s tochno izmerennymi massami (dvoinyh radiopul'sarah) massy neitronnyh zvezd lezhat v intervale 1.25-1.44Mo. Est' dve rentgenovskie sistemy, v kotoryh neitronnye zvezdy vozmozhno imeyut bOl'shuyu massu, eto Vela X-1, massa neitronnoi zvezdy v kotoroi predpolagaetsya ravnoi 1.9Mo ili dazhe 2.2Mo, i Sistema 4U110-37, gde massa neitronnoi zvezdy ocenivaetsya v 2.4Mo (dlya obeih poslednih sistem tipichnoe znachenie 1.4Mo vyhodit za 2σ). Vtoroi pik sostavlyayut kandidaty v chernye dyry. Ih massy lezhat ot 4Mo i vyshe. A v intervale ot 2.4 do 4Mo neizvestno nikakih kompaktnyh ob'ektov.

No eta situaciya, pohozhe, mozhet izmenit'sya. V sisteme 2S0921-630 (V395 Car) massa kompaktnogo ob'ekta lezhit v intervale 2.0-4.3Mo (1σ), t.e., vozmozhno, zapolnyaet ukazannyi interval. Naibolee veroyatnoe znachenie massy Kompaktnogo ob'ekta v etot sisteme 2.9Mo, takim obrazom eto mozhet okazat'sya kak ochen' massivnaya neitronnaya zvezda, tak i malomassivnaya chernaya dyra (2.9Mo prevyshaet maksimal'nuyu vozmozhnuyu massu neitronnoi zvezdy dlya bol'shinstva uravnenii sostoyaniya neitronnogo veshestva.

Orbital'nyi period sistemy 2S0921-630 sostavlyaet P=9.0035+/-0.0029 dlya, ostal'nye podrobnosti vy mozhete naiti v samoi stat'e.


Vypusk 85. 13-19 sentyabrya 2004

astro-ph/0409408 Vyzhivanie diskov vokrug radiopul'sarov (Disks Surviving the Radiation Pressure of Radio Pulsars)
Authors: K.Y. Eksi and M.A. Alpar
Comments: accepted by Astrophysical Journal

Potok izlucheniya ot radiopul'sara vovse ne obyazan razrushit' okruzhayushii ego disk. V dannoi oblasti za poslednie desyatiletiya vyshlo vsego neskol'ko teoreticheskih rabot, s kotorym avtory sravnivayut svoi rezul'taty. Vyvod avtorov takov: nesmotrya na mnenie predshestvennikov, diski vokrug radiopul'sarov mogut sushestvovat' dazhe v radiacionno-dominirovannoi zone. Pri etom oni mogut imet' slozhnuyu iskrivlennuyu formu iz-za vzaimodeistviya s magnitnym polem neitronnoi zvezdy.


Vypusk 84. 01-12 sentyabrya 2004

astro-ph/0409020 Fundamental'naya fizika i SKA: proverka gravitacii v sil'nom pole ispol'zuya pul'sary i chernye dyry (Fundamental Physics with the SKA:Strong-Field Tests of Gravity Using Pulsars and Black Holes)
Authors: M. Kramer
Comments: Talk presented at 'Exploring the Cosmic Frontier - Astrophysical Instrument for the 21st Century', to be published in Springer series "ESO Astrophysics Symposia", 4 pages, 1 figure

SKA - planiruemyi radioteleskop. Eto budet samoe moshnoe orudie radioastronomii, kogda libo sozdannoe na Zemle. Nedavno proshla konferenciya, posvyashennaya etomu proektu, a potomu v Arhive poyavlyaetsya mnozhestvo statei na etu temu. Pered vami odna iz nih.

Osnovnoi upor avtor delaet na gryadushie issledovaniya dvoinyh radiopul'sarov, gde vtorym komponentom yavlyaetsya chernaya dyra. Vladimir Lipunov i ego gruppa eshe 10-20 let nazad provodila raschety, pokazavshie, chto takie sistemy dolzhny vstrechat'sya primerno raz na neskol'ko tysyach otkrytyh radiopul'sarov. Seichas izvestno bolee 1000 radiopul'sarov. SKA budet videt' prakticheski vse pul'sary v Galaktike, chei luch voobshe popadaet na Zemlyu. Poetomu sistemy pul'sar+dyra neizbezhno budut otkryty. Kramer v svoei rabote rassuzhdaet o tom, kakie dannye, vazhnye s tochki zreniya fundamental'noi fiziki, mozhno budet poluchit' issleduyu takuyu ekzoticheskuyu paru.


astro-ph/0409204 Scintillyacii pul'sara J0737-3039A vo vremya zatmeniya (Probing the Eclipse of J0737-3039A with Scintillation)
Authors: W.A.Coles et al.
Comments: 6 pages, 7 figures, submitted to ApJ

Neskol'ko zamechanii po suti dannoi stat'i: 1). J0737-3039A samyi populyarnyi na segodnya dvoinoi radiopul'sar: obe komponenty etoi sistemy yavlyayutsya pul'sarami (odin A millisekundnym, drugoi B "obychnym"), orbital'nyi period etogo pul'sara samyi korotkii iz vseh izvestnyh, krome togo my smotrim na etu sistemu pochti s rebra.

2). I pul'sar, i Zemlya dvizhutsya v prostranstve, v rezul'tate chego luch zreniya peresekaet neodnorodnosti mezhzvezdnoi sredy. Refrakciya gigagercovogo izlucheniya pul'sarov na etih neodnorodnostyah privodit k izmeneniyu registriruemoi na Zemle intensivnosti izlucheniya pul'sara. Ukazannyi effekt nazyvaetsya mezhzvezdnymi scintillyaciyami izlucheniya pul'sarov. Po chastote podobnyh pul'sacii v svoe vremya opredelyali prostranstvennuyu skorost' etih istochnikov (izmeryayut i seichas, no mezhkontinental'naya radiointeferometriya delaet eto tochnee).

3). Razmer neitronnoi zvezdy okolo 10 km i, konechno, dve takie zvezdy v sisteme J0737-3039 ne zatmevayut drug druga neposredstvenno. Pod "zatmeniyami" v etoi sisteme podrazumevayutsya momenty vremeni, kogda izluchenie millisekundnogo komponenta J0737-3039A (on v etot moment raspolozhen szadi) prohodit skvoz' protyazhennuyu magnitosferu vtorogo komponenta J0737-3039B. Uzhe obnaruzhen celyi ryad vpolne nablyudaemyh v radiodiapazone effektov podobnogo "magnitnogo" zatmeniya.

Nablyudeniya na chastotah 820 i 1440 MGc na teleskope Grin Benk pokazali, chto scintillyacii izlucheniya oboih komponentov v moment zatmeniya stanovitsya ochen' sil'no skorrelirovannymi. Eto pozvolyaet ocenit' rasstoyanie mezhdu komponentami sistemy v kartinnoi ploskosti v moment ih maksimal'nogo sblizheniya, kak d=4000+/-2000 km, a naklonenie orbity, sootvetstvenno, kak i=90.26+/-0.13o (samoe tochnoe na segodnyashnii den' opredelenie!).


Vypusk 83. 01-31 avgusta 2004

astro-ph/0408297 Dvoinoi pul'sar J0737-3039: modulyaciya izlucheniya komponenta A pri zatmenii komponentom B (The Double Pulsar System J0737-3039: Modulation of A by B at eclipse)
Authors: M.A.McLaughlin et al.
Comments: 4 pages, 4 figures, submitted to ApJ Letters

U samogo tesnogo dvoinogo radiopul'sara PSR J0737-3039 obnaruzhen eshe odin effekt: kogda 23-millisekundnyi komponent J0737-3039A zatmevaetsya protyazhennoi magnitosferoi komponenta J0737-3039B, yavlyayushegosya normal'nym radiopul'sarom, nablyudaetsya dopolnitel'naya modulyaciya izlucheniya zatmevaemogo istochnika. Eto proyavlyaetsya v sil'noi modulyacii potoka izlucheniya v impul'sah s 2.8-sekundnym periodom vrasheniya vtorogo komponenta. Nablyudeniya velis' na chastote 820 MGc na radioteleskope Green Bank.

Eto eshe odin vid modulyacii, obnaruzhennyi u dannogo pul'sara (predydushii byl opisan v preprinte astro-ph/0407265).


astro-ph/0408356 Sobstvennoe dvizhenie odinochnoi neitronnoi zvezdy RX J1605.3+3249 (The proper motion of the isolated neutron star RX J1605.3+3249)
Authors: C. Motch et al.
Comments: 9 pages, 6 figures, accepted in A&A

U odinochnoi neitronnoi zvezdy RX J1605.3+3249 na teleskope Subaru (nablyudeniya 1999 i 2003 gg.) obnaruzheno ochen' vysokoe sobstvennoe dvizhenie: μ=144.5+/-13.2x10-6 "/god. Vyvody: skoree vsego eto blizkii ob'ekt s ochen' vysokoi prostranstvennoi skorost'yu, sledovatel'no temp akkrecii na nego nizok i ne mozhet ob'yasnit' vysokuyu nablyudaemuyu svetimost'. Takim obrazom, RX J1605.3+3249, skoree vsego, molodaya (105-106 let) goryachaya neitronnaya zvezda.


astro-ph/0408366 Millisekundnye i dvoinye pul'sary, kak estestvennye standarty chastoty (Millisecond and Binary Pulsars as Nature's Frequency Standards. III. Fourier Analysis and Spectral Sensitivity of Timing Observations to Low-Frequency Noise)
Authors: Sergei M. Kopeikin, Vladimir A. Potapov
Comments: 25 pages, 3 figures, accepted to MNRAS

Ideya ispol'zovat' radiopul'sary dlya postroeniya pul'sarnoi shkaly vremeni byla vyskazana vskore posle obnaruzheniya ochen' stabil'nyh millisekundnyh pul'sarov. Togda zhe bylo pokazano, chto shkala, osnovannaya na samyh stabil'nyh millisekundnyh pul'sarah, budet bolee stabil'noi, chem atomnaya na intervalah vremeni mesyac i bolee. Dannoe utverzhdenie ostaetsya vernym i segodnya.

V ukazannom preprinte rassmatrivayutsya razlichnye tipy shumov u odinochnyh i dvoinyh millisekundnyh pul'sarov.


astro-ph/0408439 Asimmetriya sverhnovyh i kik pul'sarov (Supernova Asymmetries and Pulsar Kicks -- Views on Controversial Issues)
Authors: H.-Th. Janka et al.
Comments: 10 pages, 5 figures

Zametka izvestnoi nemeckoi gruppy issledovatelei. Dvuh- i treh-mernye chislennye raschety pokazyvayut, chto pri vzryvah sverhnovyh voznikayut nizkomodovye (l=1,2) neustoichivosti na stadii moshnogo neitrinnogo izlucheniya. Podobnaya asimmetriya pozvolyaet neitronnoi zvezde priobresti prostranstvennuyu skorost', prevyshayushuyu 1000 km/s. Dlya vozniknoveniya ukazannyh neustoichivostei bystroe vrashenie protoneitronnoi zvezdy ne trebuetsya (i dazhe protivopokazano). [Poslednii vyvod protivorechit nablyudaemoi u radiopul'sarov sonapravlennosti osei vrasheniya i prostranstvennoi skorosti.]

Avtory takzhe govoryat, chto bimodal'nost' raspredeleniya pul'sarov po skorostyam estestvennym obrazom nahodit svoe ob'yasnenie, esli svyazat' vysokoskorostnye pul'sary s neustoichivost'yu s dominantoi l=1, a nizkoskorostnye - s l=2.


astro-ph/0408459 Skorosti vrasheniya i magnitnye polya millisekundnyh pul'sarov (Spin Rates and Magnetic Fields of Millisecond Pulsars)
Authors: Frederick K. Lamb and Wenfei Yu
Comments: 12 pages, 4 figures

Rech' idet o rentgenovskih millisekundnyh pul'sarah. Analiz ih nablyudenii s borta rentgenovskoi observatorii XMM-Newton, pokazal, chto pul'sacii vseh 16 izvestnyh ob'ektov dannogo klassa soglasuyutsya s magnitnymi polyami na poverhnosti 3x107-3x108 Gs i tempom akkrecii ot 0.001-1 Eddingtonovskogo. Takie parametry obespechivayut dlitel'nuyu stadiyu akkrecionnogo uskoreniya v malomassivnyh dvoinyh sistemah i pozvolyayut rentgenovskim millisekundnym pul'saram v posledstvii prevratit'sya v dvoinye millisekundnye radiopul'sary. No dazhe posle takoi dlitel'noi akkrecii neitronnye zvezdy ne dostigayut ravnovesnogo perioda vrasheniya!


Vypusk 82. 01-31 iyulya 2004

obzor astro-ph/0407155 Strannoe kvarkovoe veshestvo i kompaktnye zvezdy (Strange Quark Matter and Compact Stars)
Authors: Fridolin Weber
Comments: 58 figures, to appear in "Progress in Particle and Nuclear Physics"

Bol'shoi obzor, posvyashennyi razlichnym astrofizicheskim proyavleniyam kvarkovogo veshestva, v pervuyu ochered' kompaktnym zvezdam.

Obzor rasschitan na specialistov, a potomu polon lagranzhianov i prochih dlinnyh formul. Odnako razdely, posvyashennye nablyudeniyam i eksperimentam budut interesny i dostupny shirokomu krugu chitatelei. Nam bylo osobenno interesno pochitat' o poiskah strannogo veshestva v kosmicheskih luchah, a takzhe o poiskah seismicheskih yavlenii, vyzyvaemyh gipoteticheskim prohozhdeniem kapli strannoi materii (strapel'ki) cherez Zemlyu.


astro-ph/0407180 Molodye pul'sary tipa Kraba i moshnye rentgenovskie istochniki v oblastyah zvezdoobrazovaniya i v opticheski neyarkih galaktikah (Young Crab-like pulsars and luminous X-ray sources in starbursts and optically dull galaxies)
Authors: Rosalba Perna, Luigi Stella
Comments: 17 pages, 4 figures, accepted to ApJ

Zagadka ul'tramoshnyh istochnikov do sih por ne reshena. Predlagayutsya samye raznye modeli, i vot eshe odna.

Avtory rassmatrivayut gipotezu o tom, chto moshnymi rentgenovskimi istochnikami mogut byt' molodye radiopul'sary s periodami 2-9 millisekund i magnitnymi polyami (0.4-8) 1012 Gs. Ocenki pokazyvayut, chto okolo 0.3 procentov galaktik tipa nashei mogut imet' radiopul'sar s rentgenovskoi svetimost'yu vyshe 1040 erg/s. V sluchae zhe galaktiki s moshnym zvezdoobrazovaniem chastota vstrechaemosti moshnyh pul'sarov rezko vozrastaet. T.o., polagayut avtory, sredi ul'tramoshnyh istochnikov mogut byt' i takie "zveri".

Otmetim ot sebya, chto vyvody avtorov sushestvenno zavisyat ot ryada predpolozhenii. V pervuyu ochered' ot raspredeleniya nachal'nyh parametrov neitronnyh zvezd (i avtory sami eto obsuzhdayut). Dlya sushestvovaniya dostatochnogo kolichestva molodyh pul'sarov s nuzhnymi parametrami neobhodimo obespechit' rozhdenie neitronnyh zvezd s ochen' malymi periodami. Zdes' sushestvuyut problemy. Vse izvestnye nachal'nye periody vrasheniya pul'sarov prevoshodyat 10 millisekund. Vozmozhno, chto eto svyazano s t.n. r-modami, v rezul'tate razvitiya kotoryh molodaya neitronnaya zvezda bystro zamedlyaetsya, izluchaya gravitacionnye volny. Nekotorye issledovaniya pokazyvayut, chto kvarkovye zvezdy ne podverzheny etomu vidu neustoichivosti. Veroyatno, chto tol'ko molodye kvarkovye zvezdy mogut imet' dostatochno korotkie periody vrasheniya.


astro-ph/0407265 Dvoinoi pul'sar J0737-3039: Modulyaciya izlucheniya komponenta A izlucheniem komponenta B (The Double Pulsar System J0737-3039: Modulation of the radio emission from B by radiation from A)
Authors: M.A. McLaughlin et al.
Comments: 4 pages, 5 figures, Submitted to ApJ Letters

Tonkaya i krasivaya rabota: analiz povedeniya detalei profilya (subimpul'sov) normal'nogo (ne millisekundnogo) komponenta dvoinogo pul'sara PSR J0737-3039B pokazal, chto v nih proishodyat izmeneniya, kogda na magnitosferu pul'sara padaet potok izluchenii ot millisekundnogo komponenta etoi sistemy (PSR J0737-3039A). Zaregistrirovannaya chastot fluktuacii etih impul'sov v tochnosti ravna raznosti chastot pul'sarov. Nablyudeniya velis' na teleskope Green Bank na chastotah 820 i 1400 MGc.


astro-ph/0407312 Pervoe nablyudenie relyativistskogo dvoinogo pul'sara PSR J0737-3039 s XMM (A first XMM-Newton look at the relativistic double pulsar PSR J0737-3039)
Authors: A. Pellizzoni et al.
Comments: 14 pages, 3 postscript figures. Accepted in ApJL

Dannaya stat'ya - rezul'tat 50,000 sekund nablyudeniya relyativistskogo dvoinogo pul'sara PSR J0737-3039 s borta rentgenovskoi observatorii XMM-Newton v marte etogo goda. Istochnik imeet myagkii spektr (s pokazatelem stepeni =3.5(+0.5,-0.3)) i svetimost'yu v diapazone 0.2-10 keV poryadka 3x1030 erg/s (svetimost' rasschitana dlya rasstoyaniya do pul'sara ravnogo 500 pk). Ne obnaruzheny variacii ni na orbital'noi chastote (2.4 chasa), ni na chastote millisekundnogo pul'sara (22 ms).


astro-ph/0407402 Fazovaya spektroskopiya Gemingi pokazala nalichie vrashayushihsya pyaten (Phase-resolved spectroscopy of Geminga shows rotating hot spot(s))
Authors: P.A. Caraveo et al.
Comments: Published in Science, 16 July 2004

Na segodnyashnii den' Geminga schitaetsya pul'sarom, kotoryi svetit (v radio) mimo nas. A pul'sary mogut izluchat' v rentgenovskom diapazone libo za schet processov v magnitosfere (i togda izluchenie budet neteplovym), libo za schet vysokoi temperatury poverhnosti neitronnoi zvezdy. Poskol'ku pul'sar vrashaetsya, forma spektra budet periodicheski izmenyat'sya.

Nablyudeniya, proizvedennye na XMM, pokazali, chto v spektr est' teplovoi komponent ot vsei poverhnosti zvezdy (s maksimumom na 43 eV), stepennoi hvost, tyanushiisya do 2 keV. Krome togo obnaruzhen bolee goryachii teplovoi komponent (s maksimumom na 170 eV), izluchayushiisya iz oblasti diametrom okolo 60 metrov, veroyatno ih polyarnoi shapki.


Vypusk 81. 20-30 iyunya 2004

astro-ph/0406465 Orbital'nyi period ul'trakompaktnoi malomassivnoi rentgenovskoi dvoinoi sistemy 4U1543-624 (The Orbital Period of the Ultracompact Low-Mass X-Ray Binary 4U1543-624)
Authors: Z. Wang and D. Chakrabarty
Comments: 4 pages, submitted to ApJ

Orbital'nyi period dannoi sistemy byl opredelen po fotometricheskim nablyudeniyam (cherez postroenie krivoi bleska) na 6.5-m teleskope Magellan II v Chili. Etot period sostavil

18.2+/-0.1 min.

Esli, kak predpolagalos' ranee, eta sistema sostoit iz neitronnoi zvezdy, na kotoruyu istekaet zapolnyayushii polost' Rosha belyi karlik, to ego radius dolzhen sostavlyat' 0.03 Ro, a massa, sootvetstvenno, 0.03 Mo.


astro-ph/0406521 Analiz pul'sacii yader massivnyh zvezd v svyazi c pul'sarnymi kikami (Pulsational Analysis of the Cores of Massive Stars and its Relevance to Pulsar Kicks)
Authors: Jeremiah Murphy et al.
Comments: 32 pages including 12 color figures and 2 tables, submitted to ApJ

"Mnogo divnogo na svete ..."
Mnogo neponyatnogo v svyazi s rozhdeniem neitronnyh zvezd. V chastnosti, neizvestno po kakoi takoi prichine eti ob'ekty priobretayut gigantskie skorosti. Prichem, raspredelenie po skorostyam dovol'no hitroe, sostoyashee iz dvuh komponent. V pervom pike s maksimumom na 12-130 km/s nahoditsya okolo treti zvezd. Vo vtorom (s maksimumom na 700 km/s) - ostal'nye dve treti. Kak poluchit' takuyu bimodal'nost' i stol' bol'shie skorosti dlya dvuh tretei neitronnyh zvezd - neyasno.

Naibolee prorabotannoi model'yu vzryva sverhnovoi yavlyaetsya gidrodinamicheskaya. Sdelat' tam bol'shie skorosti (do 1000 km/s) dovol'no trudno (hotya Scheck et al. smogli poluchit' skorosti vyshe 500 km/s). V 1997 g. gruppa avtorov (Goldreich et al.) predpolozhili, chto iznachal'naya asimmetriya mozhet byt' svyazana s neustoichivostyami yadra zvezdy-predsverhnovoi. V etoi stat'e Merfi i dr. issleduyut v detalyah takie neustoichivosti.

Osnovnoi vyvod takov: harakternoe vremya rosta neustoichivostei slishkom veliko, chtoby uspet' kak-to sushestvenno povliyat' na vzryv.

Esli vse-taki tak i ne udastsya poluchit' vysokie skorosti v gidrodinamicheskoi modeli, to eto budet ser'eznoi problemoi ....


dissertaciya astro-ph/0406522 Radiopul'sary (Radio Pulsars)
Authors: Joeri van Leeuwen
Comments: PhD Thesis, Utrecht University 2004, with a summary in Dutch. 108 pages, 55 low-resolution figures. High-resolution versions are available at http://www.astro.uu.nl/~jleeuwen/phd_thesis/

Interesno sravnivat' dissertacii v raznyh stranah i universitetah. Oni ochen' raznye. Prakticheski vse raboty, vypolnennye v Niderlandah, kotorye nam popadalis' imeyut ochen' prostoi vid: eto prosto slozhennye poporyadku neskol'ko original'nyh statei, plyus nebol'shoe vvedenie. Imenno tak i vyglyadit dannyi trud: 4 stranicy vvedeniya i sem' statei. Stat'i dovol'no interesnye.


astro-ph/0406528 Ochen' molodoi radiopul'sar J1357-6429 (The Very Young Radio Pulsar J1357-6429)
Authors: F. Camilo et al.
Comments: Accepted for publication in ApJ Letters; 6 pages, 2 included EPS figures

V rezul'tate prodolzhayusheisya obrabotki dannyh Parksovskogo obzora otkryt eshe odin interesnyi radiopul'sar. J1357-6429 nahoditsya na rasstoyanii 2.5 kpk ot nas i vhodit v desyatku samyh molodyh pul'sarov. Vozrast ocenen v 7300 let (napomnim, chto eta velichina poluchaetsya deleniem poloviny nablyudaemogo perioda na temp zamedleniya). U etogo pul'sara uzhe obnaruzhen glitch (t.e. sboi perioda), chto podtverzhdaet ego molodost'. Ryadom s pul'sarom est' ostatok sverhnovoi G309.8-2.6.


astro-ph/0406580 Tri novyh rentgenovskih pul'sara v Malom Magellanovom Oblake (Three new X-ray pulsars detected in the Small Magellanic Cloud and the positions of two other known pulsars determined)
Authors: W.R.T.Edge et al.
Comments: Accepted by MNRAS

Korotko: po dannym RXTE v Malom Magellanovom Oblake zaregistrirovany eshe tri rentgenovskih pul'sara. Ih periody: 34, 503 i 138 sekund.


Vypusk 80. (01) - 12-20 iyunya 2004

astro-ph/0406321 Orbital'naya modulyaciya nablyudaemoi mery dispersii pul'sara PSR J0737-3039A (Orbital Modulation of the Apparent Dispersion Measure Towards PSR J0737-3039A)
Authors: Scott M. Ransom et al.
Comments: 4 pages, 0 figures, submitted to ApJ Lett.

PSR J0737-3039 - sistema, sostoyashaya iz dvuh vidimyh s Zemli radiopul'sarov. Komponent PSR J0737-3039A - millisekundnyi komponent etoi sistemy.

Regulyarnye nablyudeniya etoi sistemy pokazali, chto mera dispersii (DM - kolichestvo elektronov na luche zreniya) periodicheski menyaetsya pri dvizhenii pul'sara po orbite. Amplituda etoi modulyacii sostavlyaet primerno 0.09 pk/sm3. Maksimumy (i minimumy) DM prihodyatsya primerno na maksimal'nye elongacii (polozheniya, kogda pul'sary razdelyaet maksimal'noe uglovoe rasstoyanie). Variaciya mery dispersii korelliruyut s rasstoyaniem pul'sara ot centra mass sistemy.


Vypusk 78. 13-31 maya 2004

populyarnyi obzor astro-ph/0405262 Fizika neitronnyh zvezd (The Physics of Neutron Stars)
Authors: J.M. Lattimer, M. Prakash
Comments: 22 pages, 4 figures and 1 table. Science Vol. 304 2004 (536-542)

Zhalko, chto v Rossii net analoga zhurnala Science.

V Arhive poyavilsya ocherednoi obzor, napisannyi dlya Science. Stil' zhurnala obyazyvaet avtorov izlagat' strogo, no ponyatno dlya nespecialistov v konkretnoi uzkoi oblasti.

Stat'ya ohvatyvaet osnovnye aspekty fiziki neitronnyh zvezd (vklyuchaya i kvarkovye zvezdy). Konechno, avtory rasskazyvayut i o svezhih nablyudatel'nyh dannyh. Otmetim nalichie poleznyh tablic, simpatichnyh risunkov i mnozhestva ssylok.


astro-ph/0405311 Krupnomasshtabnaya anizotropiya pri vzryve sverhnovyh i skorosti pul'sarov (Global Anisotropies in Supernova Explosions and Pulsar Recoil)
Authors: L. Scheck et al.
Comments: 3 pages, 2 figures, contribution to Procs. 12th Workshop on Nuclear Astrophysics, Ringberg Castle, March 22-27, 2004

Korotkaya zametka v trudah konferencii, yavlyayushayasya kratkim izlozhenie stat'i teh zhe avtorov, opublikovannoi ranee v etom godu v Phys. Rev. V dvuh slovah rezul'taty mozhno summirovat' tak: avtoram (po suti vpervye) udalos' poluchit' vysokuyu skorost' otdachi (kik) v modeli obychnogo gidrodinamicheskogo (s neitrino konechno) vzryva sverhnovoi.


astro-ph/0405364 Parksovskii obzor pul'sarov: IV. Otkrytie 180 pul'sarov i parametry dlya 281 ranee izvestnogo pul'sara (The Parkes multibeam pulsar survey: IV. Discovery of 180 pulsars and parameters for 281 previously known pulsars)
Authors: G. Hobbs et al.
Comments: 35 pages, accepted for publication in MNRAS, a high quality image of the figure on page 32 is available from http://www.atnf.csiro.au/research/pulsar/images/pmsurvey_fig.ps

Ocherednaya stat'ya, posvyashennaya vazhneishemu dlya astrofiziki neitronnyh zvezd proektu - Parksovskomu obzoru.

Obzor provodilsya na treh instrumentah: 64-metrovom Parkse, 305-metrovom teleskope v Aresibo i 76-metrovom Lovellovskom teleskope. Otkryto bolee 700 novyh pul'sarov. S uchetom nablyudenii ranee izvestnyh istochnikov katalog pozvolyaet poluchit' odnorodnye dannye po bolee chem 1000 radiopul'sarov.

Krome mnozhestva dannyh (tabliciy, risunki) avtory privodyat bolee podrobnye raz'yasneniya po otdel'nym naibolee vydayushimsya istochnikam (o mnogih uzhe rasskazyvalos' otdel'no, i sootvetstvenno my pisali o nih v obzorah).


astro-ph/0405559 Reviziya radial'nogo raspredeleniya pul'sarov v Galaktike (Revisiting the radial distribution of pulsars in the Galaxy)
Authors: I. Yusifov, I. Kucuk
Comments: 9 pages, 5 figures, 3 tables, LaTeX2e, Accepted for publication in A&A

Interesnaya stat'ya, posvyashennaya raspredeleniyu radiopul'sarov v Galaktike. Avtory ispol'zovali poslednie dannye, vklyuchayushie bolee 1000 radiopul'sarov (analogichnaya rabota po drugoi metodike takzhe byla provedena Lorimerom, sm. astro-ph/0308501).


Proekciya raspredeleniya radiopul'sarov na ploskost' Galaktiki. Centr Galaktiki nahoditsya v nachale koordinat. Solnce - v tochke X=0, Y=8.5. Novye pul'sary (iz poslednego obzora) pokazany krestikami, starye (izvestnye ranee) - tochkami. Serym pokazany spiral'nye rukava.

Vidny dve osobennosti:
Vokrug nas lokal'no mnogo pul'sarov, no chut' dal'she ot Solnca pul'sarov uzhe men'she (eto mozhet byt' svyazano s Poyasom Gulda).
Pul'sarov v central'noi oblasti Galaktiki malo (etot effekt ne svyazan prosto s tem, chto centr daleko, i nablyudat' tam neprosto).


Radial'noe raspredelenie nablyuademyh pul'sarov (t.e. ne dobavlen effekt t.n. "biminga", s uchetom effekta, svyazannogo s tem, chto luch pul'sara mozhet ne popadat' na Zemlyu, kolichestvo uvelichitsya v 4-10 raz).

Bezuslovno, takuyu vazhnuyu rabotu budut povtoryat' nezavisimo i drugie gruppy. Budem zhdat', chtoby sravnit' rezul'taty. Poka zhe eta rabota (plyus stat'ya Lorimera) - eto samoe poslednee, chto est' po raspredeleniyu pul'sarov v Galaktike.


astro-ph/0405564 Galakticheskii temp sliyaniya dvoinyh neitronnyh zvezd: naibolee svezhie ocenki (The Galactic Double-Neutron-Star Merger Rate: Most Current Estimates)
Authors: Chunglee Kim et al.
Comments: 8 pages, 3 figures, to appear in proceedings of Aspen Center for Physics Conference on ``Binary Radio Pulsars'' Eds. F. Rasio and I. Stairs. New results on the systematic uncertainties and possible upper limits on rate estimates are included

Proshlogodnee otkrytie dvoinogo radiopul'sara povliyalo na ocenki tempa sliyaniya dvoinyh neitronnyh zvezd. Tochnee skazat' tak. Chisto teoreticheskie ocenki, osnovannye na scenariyah evolyucii dvoinyh, lish' poluchili nakonec podtverzhdenie. A vot ocenki, gde klyuchevuyu rol' igralo nablyudaemoe kolichestvo sistem, kotorye mogut slit'sya na vremya zhizni Vselennoi, izmenilis' v storonu uvelicheniya chastoty sliyanii. Delo v tom, chto novootkrytaya sistema a) blizkaya, b) sol'etsya bystro, v) pul'sary ne ochen' yarkie. Eto oznachaet, chto takih sistem dolzhno byt' dovol'no mnogo.

V etoi rabote avtory kratko obsuzhdayut kakovy novye ocenki, i voobshe, chto izmenilos' v etoi oblasti astrofiziki za samoe poslednee vremya.


Vypusk 76. 19-30 aprelya 2004

astro-ph/0404341 Issledovaniya dvoinogo pul'sara PSR J0737-3039 na teleskope v Grin Benk (GBT Exploratory Time Observations of the Double-Pulsar System PSR J0737-3039)
Authors: S. Ransom et al.
Comments: 9 pages, including 8 figures. To appear in proceedings of Aspen Center for Physics Conference on `Binary Radio Pulsars'' Eds. F. Rasio and I. Stairs

Sistema dvoinogo radiopul'sara PSR J0737-3039 ochen' vazhna dlya fiziki i astrofiziki. Poetomu istochniki (t.e. oba pul'sara) aktivno nablyudayut i regulyarno rasskazyvayut o novyh rezul'tatah. Imenno etomu i posvyashena dannaya zametka.

Sm. takzhe stat'yu "Fluctuation and morphological properties of the pulsars in J0737--3039 system" (astro-ph/0404392)


astro-ph/0404423 Pul'sarnye kiki i otkloneniya osei vrasheniya v tesnyh dvoinyh sistemah neitronnyh zvezd PSR J0737-3039, PSR B1534+12 and PSR B1913+16 (Pulsar Kicks and Spin Tilts in the Close Double Neutron Stars PSR J0737-3039, PSR B1534+12 and PSR B1913+16)
Authors: B. Willems, V. Kalogera, M. Henninger
Comments: 25 pages, Submitted to ApJ. A version with high resolution figures may be downloaded at http://www.astro.northwestern.edu/~bart/publications.html

Avtory obsuzhdayut takoi vopros: mozhno li po dannym nablyudenii dvoinyh neitronnyh zvezd (sistemy tipa pul'sar+pul'sar ili pul'sar+nepul'siruyushaya neitronnaya zvezda) poluchit' ogranicheniya na skorosti otdachi (kiki) i na velichinu ugla mezhdu os'yu vrasheniya pul'sara i os'yu orbital'nogo momenta sistemy. I kik, i smeshenie osi po uglu voznikayut iz-za vzryva sverhnovoi. V svyazi s etim predstavlyaetsya ochen' vazhnym maksimal'no ispol'zovat' dannye nablyudenii dlya polucheniya informacii, svyazannoi s fizikoi vzryva.

V osnovnom avtory obsuzhdayut sistemu edinstvennogo "dvoinogo-dvoinogo" pul'sara (sistema iz dvuh pul'sarov). Bolee kratko rassmatrivayutsya sistemy PSR B1534+12 i PSR B1913+16 (pul'sar+neitronnaya zvezda).

Za schet novyh dannyh i rasshireniya prostranstva parametrov avtory poluchayut rezul'taty, otlichayushiesya ot bolee rannih (v tom chisle poluchennyh samimi avtorami). Ne vnikaya v detali, mozhno skazat', chto:
1. Ochen' bol'shie skorosti (bolee 1000 km/s) ne isklyucheny;
2. Ochen' malye skorosti - menee 60 dlya J0737-3039, menee 45 dlya PSR B1534+12 i menee 190 dlya PSR B1913+16 - isklyucheny.


astro-ph/0404428 X1908+075: Pul'sar, vrashayushiisya v zvezdnom vetre massivnogo kompan'ona (X1908+075: A Pulsar Orbiting in the Stellar Wind of a Massive Companion)
Authors: A. M. Levine et al.
Comments: 16 pages, 11 Postscript figures, submitted to ApJ

Istochnik X1908+075 izvesten eshe s samyh rannih rentgenovskih nablyudenii. Odnako opticheskogo otozhdestvleniya ne bylo i ne do ih por. Nekotoroe vremya nazad po dannym RXTE byl obnaruzhen orbital'nyi period (4.4 dnya). V etoi rabote avtory rasskazyvayut ob otkrytii perioda 605 sekund. Ochevidno, chto eto period vrasheniya neitronnoi zvezdy.

Udalos' dostatochno mnogo uznat' ob etoi sisteme. Kompan'onom yavlyaetsya massivnaya zvezda s vysokim tempom poteri massy v vide zvezdnogo vetra, prichem ne gigant. Avtory polagayut, chto eto zvezda Vol'fa-Raie. A znachit, rassuzhdayut oni, v skorom vremeni (desyatki tysyach let) ona mozhet prevratit'sya v chernuyu dyru. T.e. sistema mozhet yavlyat'sya praroditelem interesneishih (i eshe ne otkrytyh) sistem neitronnaya zvezda + chernaya dyra!


astro-ph/0404483 Pul'sarnyi kik i temnaya materiya v vide steril'nyh neitrino (Pulsar kicks and dark matter from a sterile neutrino)
Authors: Alexander Kusenko
Comments: 7 pages, 1 figure

Pri svoem rozhdenii vnutri sverhnovyh bol'shinstvo pul'sarov (neitronnyh zvezd) ispytyvayut kik ("pinok"), pod deistviem kotorogo oni priobretayut skorosti dostigayushie soten kilometrov v sekundu. Mehanizm dannogo processa na segodnya ne yasen. Predlagalis' razlichnye modeli, v chastnosti, asimmetrichnoe ispuskanie neitrino. Vse ranee predlozhennye neitrinnye mehanizmy kika byli otvergnuty (iz-za slishkom nizkih skorostei). V dannoi zametke avtor pytaetsya vozrodit' takoi mehanizm, no dlya etogo trebuetsya predpolozhit' sushestvovanie steril'nyh neitrino s massami v intervale 1-20 keV. Zaodno iz takih chasticy mogla by sostoyat' nebarionnaya temnaya materiya (ne putat' s temnoi energiei - lyambda-chlenom).

Ogranicheniya na parametry steril'nyh neitrino (massy i ugly smeshivaniya): chernaya oblast' zapreshena - v nei plotnost' neitrino vyshe 30% ot kriticheskoi plotnosti Vselennoi (t.e. bol'she, chem vsei temnoi materii). Oblasti, otmechennye ciframi "1" i "2", udovletvoryayut nablyudaemym parametram pul'sarov. Uzkaya zheltaya oblast' - dopustimye parametry v predpolozhenii, chto temnaya materiya sostoit tol'ko iz steril'nyh neitrin.


astro-ph/0404496 Trehmernoe modelirovanie diskovoi akkrecii na magnitnyi dipol': II Goryachie pyatna i peremennost' (Three-dimensional Simulations of Disk Accretion to an Inclined Dipole: II. Hot Spots and Variability)
Authors: Marina M. Romanova et al.
Comments: 15 pages, 13 figures

Iz rimskoi dvoiki v nazvanii stat'i vy mozhete ponyat', chto rech' idet o prodolzhenii cikla issledovanii, i eto deistvitel'no tak, pervaya ih chast' byla opublikovana v preprinte astro-ph/0401375. Naibolee interesnye novye vyvody avtorov takovy:

  • veshestvo padaet na poverhnost' kompaktnoi zvezdy vblizi magnitnyh polyusov, no ne ravnomerno, a obrazuet dugoobraznye pyatna;
  • temp akkrecii periodicheski izmenyaetsya (s chastotoi osevogo vrasheniya zvezdy).

V lyubom sluchae uvazhaemym chitatelyam stoit obratitsya k samoi stat'e: zhelayushim razobrat'sya - chitat', a prosto interesuyushimsya - smotret'.


Na stranice avtorov mozhno posmotret' fil'm, vypolnennyi po rezul'tatam ih raschetov.


astro-ph/0404514 Obrazovanie samogo relyativistskogo pul'sara PSR J0737-3039 (The Formation of the Most Relativistic Pulsar PSR J0737-3039)
Authors: B.Willems et al.
Comments: 6 pages, 7 figures

Prodolzhayutsya teoreticheskie issledovaniya (dvazhdy) dvoinogo pul'sara PSR J0737-3039. Vyvody takovy:

  • massa vtoroi predsverhnovoi, porodivshei molodoi sekundnyi pul'sar v etoi sisteme, lezhala v intervale ot 2.1 do 4.7 massy Solnca;
  • radius predsverhnovoi mog byt' ot 1.2 do 1.7 radiusa Solnca;
  • pul'sar ispytal kik ot 60 do 1660 km/s;
  • napravlenie kika otklonyalos' ot osi vrasheniya zvezdy ne menee, chem na 25o.


astro-ph/0404569 Geometriya dvuhpul'sarnoi sistemy J0737-3039 po sistematicheskim izmeneniyam intensivnosti izlucheniya (The geometry of the double-pulsar system J0737-3039 from systematic intensity variations)
Authors: F.A. Jenet, S.M. Ransom
Comments: 12 pages, 3 figures

Eshe odna model', ob'yasnyayushaya pochemu obychnyi (ne millisekundnyi) pul'sar (komponent "B") v etoi sisteme registriruetsya tol'ko na opredelennyh orbital'nyh fazah. V ih modeli izluchenie komponenta "B" usilivaetsya, kogda ego magnitosfera obluchaetsya komponentom "A". Takaya model' nalagaet opredelennye ogranicheniya na orientaciyu osi vrasheniya i diagrammu napravlennosti millisekundnogo pul'sara ("A"). Eta zhe model' predskazyvaet opredelennuyu evolyuciyu profilya millisekundnogo pul'sara, a takzhe tot fakt, chto iz-za geodezicheskoi precessii vsego cherez 15-20 let ego luch perestanet popadat' na Zemlyu.

Stat'ya opublikovana v zhurnale Nature 428, 919 (2004).


Vypusk 75. 12-19 aprelya 2004

astro-ph/0404213 Obzor po poisku pul'sarov v sharovyh skopleniyah na volne 20 sm (A 20-cm Survey for Pulsars in Globular Clusters using the GBT and Arecibo)
Authors: Scott Ransom et al.
Comments: 7 pages, 2 figures, to be published in the proceedings of the "Binary Pulsars" Conference, Aspen, January 2004

Seichas izvestno primerno 80 pul'sarov v 23 sharovyh skopleniyah. Pri etom bolee poloviny iz nih otkryty za poslednie 4 goda. Eto svyazano s aktivnymi poiskovymi programmami v Arecibo i Green Bank.

V etoi korotkoi zametke avtory rasskazyvayut ob otkrytii 13 millisekundnyh pul'sarov (eshe est' kandidaty). Iz nih 12 - dvoinye (iz nih tri - zatmennye). Poka obrabotano 80 procentov dannyh, obrabotka prodolzhaetsya.

Rasskaz o kazhdom novom pul'sare soprovozhdaetsya kratkoi informaciei po materinskomu sharovomu skopleniyu.


astro-ph/0404274 Para chasov v dvoinom pul'sare PSR J0737-3039: ego proishozhdenie i evolyuciya (Two clocks in the PSR J0737-3039 binary system and their implications for the system's origin and evolution)
Authors: D.R.Lorimer et al.
Comments: 4 pages, 1 figure

Ochen' korotkaya (4 stranicy) stat'ya pro to: chto mozhno uznat', nablyudaya samyi populyarnyi segodnya dvoinoi pul'sar s dvumya nablyudaemymi komponentami. A takzhe iz chego i kak on obrazovalsya.


astro-ph/0404290 Molekulyarnaya vodorodnaya atmosfera neitronnoi zvezdy (A hydrogenic molecular atmosphere of a neutron star)
Authors: A.V. Turbiner and J.C. Lopez Vieyra
Comments: 8 pages, 1 figure

Molekuly v atmosferah neitronnyh zvezd?

Okazyvaetsya eto vpolne vozmozhno. Po krainei mere dlya odinochnoi neitronnoi zvezdy 1E1207.4-5209 nailuchshee soglasie s nablyudeniyami daet model' atmosfery, v kotoroi osnovnym komponentom yavlyaetsya ekzoticheskii molekulyarnyi ion H32+ i magnitnym polem 2-6x1014 Gs.

Reakcii fotoionizacii

H32+ -> e + 3p
i fotodissociacii
H32+ -> H + 2p
pozvolyayut ob'yasnit' absorbcionnye detali na energiyah 0.7 i 1.4 keV. Krome togo dannaya model' predskazyvaet osobennost' na energii 80-150 eV iz-za drugoi reakcii fotodissociacii
H32+ -> H2+ + p.


miniobzor astro-ph/0404324 Astrofizika pul'sarov: fenomen glitchei (Pulsar astrophysics: the glitch phenomenon)
Authors: J.E. Horvath
Comments: 8 pp. 3 fig.,

Ochen' korotkii obzor pro sboi vrasheniya pul'sarov i ih mehanizmy. Naibol'shii upor avtor delaet upor na pul'sar PSR B1828-11 v kotorom, vozmozhno, nablyudaetsya svobodnaya precessiya.


Vypusk 74. 01-11 aprelya 2004

astro-ph/0404100 Pul'sarnye kiki: vrashenie i kinematika (Pulsar Kicks: Spin and Kinematic Constraints)
Authors: Roger W. Romani
Comments: 6 pages, To Appear in Proceedings of the 2004 Apsen Winter Conf. on Astrophysics, APS Conf Series, Rasio & Stairs, eds

Dlya neskol'kih pul'sarov - Kraba (sm. ris.), Vely, i eshe dvuh-treh drugih - mozhno opredelit' otnositel'noe napravlenie osi vrasheniya, magnitnoi osi i vektora prostranstvennoi skorosti. Skorosti pul'sary priobretayut posle (ili v processe) svoego rozhdeniya (eto ochevidno iz togo, chto skorosti zvezd-praroditelei namnogo men'she). Konkretnyi mehanizm, privodyashii k kiku (kick - udar, tolchok), ostaetsya neizvestnym, i zdes' lyubaya informaciya ochen' i ochen' vazhna.

Sovremennye dannye pokazyvayut, chto raspredelenie pul'sarov po skorostyam bimodal'no. Primerno polovina pul'sarov imeet skorosti poryadka 100 km/s, a vtoraya polovina - gorazdo bOl'shie (poryadka 300-700 km/s). Pul'sar v Krabovidnoi tumannosti i pul'sar v Parusah (Vela) otnosyatsya k nizkoskorostnoi populyacii. Dlya etih ob'ektov skorosti okazalis' pochti sonapravlennymi s napravleniem dvizheniya. Odnako vazhno ponyat': ili tochno sonapravleny, ili imenno chto "pochti". V etoi korotkoi zametke Rodzher Romani summiruet poslednie dannye i obsuzhdaet kakie ogranicheniya nakladyvayutsya na modeli vspyshek sverhnovyh.

Kratkoe rezyume takovo: otklonenie vektora skorosti ot osi vrasheniya sostavlyaet neskol'ko gradusov, i eto znachimyi rezul'tat. Tak chto tochnoi sonapravlennosti net, no est' ochevidnyi trend. Po mneniyu avtora eto prakticheski isklyuchaet modeli s obychnym gidrodinamicheskim kikom (t.k. tam kik napravlen haotichno), a takzhe model' elektro-magnitnoi rakety, t.k. tam kik dolzhen byt' napravlen tochno po osi. Avtor polagaet, chto kik, svyazannyi s anizotropnym izlucheniem neitrino horosho sootvetstvuet nablyudeniyam.

Ot sebya otmetim, chto ne vse tak ochevidno. Vo-pervyh, mogut rabotat' srazu dva mehanizma (naprimer, kak raz gidrodinamicheskii i elektro-magnitnaya raketa), i togda tochno sonapravlennosti ne budet, no budet trend. Vo-vtoryh est' i drugie modeli, naprimer, model' magnitorotacionnaya, gde kak raz net tochnoi sonapravlennosti (pravda, chastino ona kak raz popadaet, v smysle kika, pod anizotropnoe izluchenie neitrino). V-tret'ih, mozhet byt' velika rol' dvoistvennosti: pri raspade massivnoi dvoinoi (chto ves'ma veroyatno posle vzryva sverhnovoi) zvezdy sohranyayut orbital'nye skorosti. Nu i v-chetvertyh, poka eti rezul'taty ne kasayutsya vysokoskorostnyh pul'sarov.


astro-ph/0404102 Taiming rentgenovskih zatmenii v malomassivnoi rentgenovskoi sisteme EXO 0748-676 (X-Ray Eclipse Timing in the LMXB EXO 0748-676)
Authors: Michael T. Wolff et al.
Comments: 4 Pages, 3 Figures

Neobychnaya zatmennaya rentgenovskaya sistema EXO 0748-676 byla otkryta v 1985 godu. Za eto vremya orbital'nyi period sistemy trizhdy rezko (za ochen' korotkii interval vremeni) izmenyalsya, posle chego ostavalsya na pochti postoyannom urovne v techenie dostatochno dolgogo vremeni. Veroyatno, eto povedenie svyazano s izmeneniyami v processah perenosa veshestva v dvoinoi. Avtory detal'no issledovali povedenie orbital'nogo perioda sistemy v poslednie 18 mesyacev.

Diagramma O-S, pokazyvayushaya raznost' mezhdu nablyudaemymi momentami zatmenii (O - observation) i ih predskazannymi znacheniyami (S - calculated). Kazhdyi lineinyi uchastok sootvetstvuet intervalu vremeni, kogda orbital'nyi period sistemy byl postoyannym.


miniobzor astro-ph/0404105 Zatmennye dvoinye pul'sary (Eclipsing Binary Pulsars)
Authors: Paulo C. C. Freire
Comments: 14 pages, 5 figures, 1 table

Pervyi zatmennyi dvoinoi pul'sar PSR B1957+20 byl otkryt v 1987 godu. S toi pory bylo otkryto eshe 13 takih sistem, 12 iz kotoryh nahodyatsya v sharovyh skopleniyah. Avtory privodyat tablicu parametrov etih ob'ektov i podrobno obsuzhdayut kazhdyi, osobenno zatmennye pul'sary v sharovom skoplenii 47 Tuc.

Avtory schitayut, chto vse ob'ekty mozhno razdelit' na dve gruppy: malomassivnye kompan'ony s M~0.02Mo, veroyatno, prisutstvovali v dannyh dvoinyh s samogo nachala (t.e. oni obrazovalis' odnovremenno s massivnoi zvezdoi - praroditelem pul'sara). Vtoraya gruppa sistem: pul'sary s bolee massivnymi komponentami s M~0.2Mo - voznikla v rezul'tate dinamicheskogo obmena malomassivnoi v sisteme pul'sara pervogo tipa na bolee tyazheluyu.


obzor astro-ph/0404136 Rentgenovskie istochniki v sharovyh skopleniyah (Globular Cluster X-ray Sources)
Authors: Frank Verbunt, Walter H.G. Lewin
Comments: 39 pages, Chapter 8 in "Compact Stellar X-ray Sources", eds. W.H.G. Lewin and M. van der Klis, Cambridge University Press

Eto glava iz knigi po kompaktnym rentgenovskim istochnikam. V nei vy naidete kratkuyu istoriyu izucheniya rentgenovskih istochnikov v sharovyh skopleniyah nashei Galaktiki, rezul'taty izucheniya ochen' yarkih rentgenovskih istochnikov v 14 sharovyh skopleniyah v sosednih galaktikah, i diskussiyu o putyah i formirovaniya i shodstve (razlichiyah) s istochnikami vne sharovyh skoplenii.


astro-ph/0404144 Model' opticheskogo/IK izlucheniya ot magnitarov (A Model for the Optical/IR Emission from Magnetars)
Authors: Feryal Ozel
Comments: 10 preprint pages, 3 figures, submitted to ApJL

Na segodnyashnii den' naibolee obsheprinyatoi gipotezoi o prirode anomal'nyh rentgenovskih pul'sarov (ARP) i istochnikov povtoryayushihsya gamma-vspleskov (MPG) yavlyaetsya magnitarnaya. T.e. my imeem delo so sverhzamagnichennoi neitronnoi zvezdoi. V ramkah etoi gipotezy neploho udaetsya ob'yasnit' fenomenologiyu v zhestkih diapazonah spektra. Odnako ARP nablyudayutsya i v optike i IK (MPG ne nablyudayutsya, no eto prosto mozhet byt' svyazano s bol'shim poglosheniem). V dannoi stat'e avtor pytaetsya postroit' model' opticheskogo/IK izlucheniya magnitarov. Osnovnym vyvodom yavlyaetsya to, chto nablyudaemyi potok v etih diapazonah - eto sinhrotronnoe izluchenie, voznikayushee na rasstoyaniyah bol'shih 50 radiusov zvezdy.


astro-ph/0404149 Izmereniya skorosti dvoinogo pul'sara J0737-3039 (Green Bank Telescope Measurement of the Systemic Velocity of the Double Pulsar Binary J0737-3039 and Implications for its Formation)
Authors: S. M. Ransom et al.
Comments: 5 pages, 3 figures. To be submitted to ApJ Letters.

Po dannym radionablyudenii udalos' opredelit' prostranstvennuyu skorost' dvoinogo radiopul'sara J0737-3039 (tochnee, opredelena proekciya skorosti na nebo). Znachenie skorosti poryadka 140 km/s. Pri etom imeetsya znachitel'naya sostavlyayushaya perpendikulyarnaya ploskosti orbity sistemy. Eto ukazyvaet na to, chto vtoroi pul'sar (V) rodilsya so znachitel'nym kikom 100-200 km/s. Otmetim odnako sleduyushee: sushestvenno, chto kik vse-taki lezhit v pervom pike raspredeleniya neitronnyh zvezd po skorostyam (o bimodal'nosti raspredeleniya sm. vyshe).


astro-ph/0404159 Zondirovanie relyativistskih vetrov v pul'sare PSRJ07370-3039 A i B (Probing Relativistic Winds: The case of PSRJ07370-3039 A & B)
Authors: Jonathan Arons et al.
Comments: 11 pages, 3 figures.

U otkrytogo v konce 2003 goda dvoinogo pul'sara PSRJ07370-3039 vtoroi komponent takzhe okazalsya radiopul'sarom (teper' ih nazyvayut A i B). "Normal'nyi" (t.e. ne millisekundnyi) pul'sar PSRJ07370-3039B viden tol'ko na opredelennyh orbital'nyh fazah - v ostal'noe vremya ego izluchenie pogloshaetsya.

Okolo mesyaca nazad bylo prelozheno pervoe prostoe ob'yasnenie etogo yavleniya (sm. astro-ph/0403076). V dannoi stat'e ob'yasnenie takoe zhe: pogloshenie, no rassmotrenie gorazdo bolee detal'noe. V prelozhennoi modeli vokrug magnitosfery pul'sara "B" obrazuetsya kokon, v kotorom i proishodit pogloshenie.


Model' "kokona" vokrug magnitosfery pul'sara


astro-ph/0404167 Tri novyh dvoinyh radiopul'sara po dannym Parks (Three New Binary Pulsars Discovered With Parkes)
Authors: Jason Hessels et al.
Comments: To appear in Binary Radio Pulsars, proceedings of an Aspen Winter Conference, eds. F. Rasio, I. Stairs, 4 pages, 2 figures

S pomosh'yu mnogokanal'nogo priemnika Parks provodilis' nablyudeniya oblastei lokalizacii 56 neotozhdestvlennym gamma-istochnikov iz kataloga EGRET. Naibolee veroyatno, chto okolo poloviny iz etih istochnikov yavlyayutsya blizkimi neitronnymi zvezdami, svyazannymi s Poyasom Gulda. V dannoi korotkoi zametke dany svedeniya o treh otkrytyh dvoinyh radiopul'sarah. Po mneniyu avtorov vse tri v toi ili inoi stepeni yavlyayutsya neobychnymi ob'ektami.


astro-ph/0404174 Svoistva i interpretaciya gigantskih [mikro]impul'sov ot pul'sarov (Properties and Interpretations of Giant Micropulses and Giant Pulses from Pulsars)
Authors: Iver H. Cairns
Comments: 19 pages, 2 tables, zero figures

Vremya ot vremeni u pul'sarov nablyudayutsya gigantskie impul'sy i gigantskie mikroimpul'sy. Potok izlucheniya v nih na poryadki vyshe, chem v "obychnyh" impul'sah i mikroimpul'sah. Krome bol'shih potokov i redkosti poyavleniya gigantskie impul'sy obladayut sleduyushimi svoistvami: ih amplitudy (potoki) imeyut primerno stepennoe raspredelenie, krome togo, oni poyavlyayutsya tol'ko v opredelennyh intervalah faz pul'sara.

V stat'e privedeno opisanie statisticheskih svoistv gigantskih impul'sov i rassmatrivayutsya dva naibolee populyarnyh segodnya ob'yasneniya ih proishozhdeniya. Pervaya model' schitaet, chto vse impul'sy pul'sarov obrazuyutsya v rezul'tate stohasticheskogo narastaniya slabogo zatravochnogo vozmusheniya. V etoi modeli vse "giganty" eto hvost raspredeleniya, v kotoryi popadayut naibolee moshnye i naibolee redkie sobytiya. Drugoi variant - usilenie na fluktuaciyah prelomlyayushei sredy vnutri magnitosfery pul'sara. No eta model' men'she nravitsya avtoram.


astro-ph/0404181 Novye dvoinye i millisekundnye pul'sary po dannym Aresibo (New Binary and Millisecond Pulsars from Arecibo Drift-Scan Searches)
Authors: M. A. McLaughlin et al.
Comments: 6 pages, 3 figures, to appear in proceedings of Aspen Center for Physics Conference on `Binary Radio Pulsars'' Eds. F. Rasio and I. Stairs

Obsuzhdayutsya chetyre "podkruchennyh" radiopul'sara (dva dvoinyh i dva odinochnyh), otkrytyh na teleskope v Aresibo. Krome opisaniya chetyreh interesnyh ob'ektov (daleko ne vse novye pul'sary vydelyayut v otdel'nye publikacii) avtory privodyat neskol'ko interesnyh grafikov i obsuzhdayut nereshennye problemy. Otmetim odnu iz nih.

Kak rozhdayutsya odinochnye millisekundnye radiopul'sary? Est' dve idei: ili razrushenie (isparenie) vtorogo komponenta, ili sliyanie dvuh belyh karlikov. Est' interesnye dannye (pravda, na ne ochen' bol'shoi vyborke), chto prostranstvennaya skorost' odinochnyh millisekundnyh radiopul'sarov men'she skorosti dvoinyh (primerno 60 km/s protiv 120). Znachit ....


Vypusk 73. 16-31 marta 2004

astro-ph/0403453 Otkrytie millisekundnogo radiopul'sara v ochen' ekscentrichnoi dvoinoi sisteme (GMRT Discovery of A Millisecond Pulsar in a Very Eccentric Binary System)
Authors: Paulo C. Freire et al.
Comments: 12 pages (referee format), 3 figures, accepted for publication in Astrophysical Journal Letters

Otkryt dvoinoi millisekundnyi radiopul'sar v sharovom skoplenii NGC 1851. Vazhnoi osobennost'yu sistemy yavlyaetsya ee bol'shoi ekscentrisitet - 0.89.

Sovetuem prochest' i obratit' vnimanie na ideyu avtorov o tom, chto kompan'onom pul'sara mozhet byt' chernaya dyra!


miniobzor astro-ph/0403489 Svoistva neitronnyh zvezd (Properties of neutron stars)
Authors: M. H. van Kerkwijk (Univ. of Toronto)
Comments: 12 pages, 2 figures

U neitronnyh zvezd dostatochno mnogo raznyh svoistv. V etoi stat'e avtor obrashaet osnovnoe vnimanie na ih maksimal'nye massy i radiusy.


astro-ph/0403553 PSR J1829+2456: relyativistskii dvoinoi pul'sar (PSR J1829+2456: a relativistic binary pulsar)
Authors: D. J. Champion et al.
Comments: Accepted MNRAS, 5 pages, 3 figures

Korotko: otkryta eshe odna sistema radiopul'sar + neitronnaya zvezda.

V otlichii ot nashumevshego "istinno dvoinogo radiopul'sara" - sistemy, gde obe neitronnye zvezdy dayut impul'sy - novaya sistema soderzhit lish' odin aktivnyi ob'ekt (hotya, kto znaet, vozmozhno v budushem udastsya chto-to eshe razglyadet'). Eto sed'maya takaya sistema.

Sistema byla otkryta po dannym teleskopa v Aresibo. Nablyudeniya provodilis' azh v 1999 g., no obrabotka byla zakonchena lish' nedavno. Krome togo, v 2003 g. na toi zhe apparature provodilis' povtornye nablyudeniya, podtverdivshie fakt otkrytiya. Zatem provodilis' dopolnitel'nye nablyudeniya dlya opredeleniya parametrov dvoinoi.

Pul'sar imeet period okolo 41 millisekundy. Period dvoinoi - 28 chasov. Ekscentrisitet - 0.14 Takaya sistema sol'etsya za schet izlucheniya gravvoln lish' cherez 60 milliardov let, tak chto novoe otkrytie ne okazalo vliyaniya na raschety tempa registracii gravitacionno-volnovyh vspleskov.

Polozhenie pul'sara na nebe ukazyvaet, chto on mozhet prinadlezhat' nashemu lyubimomu Poyasu Gulda.

Massa pul'sara ne bolee 1.38 massy solnca, massa kompan'ona - primerno mezhdu 1.22 i 1.38 (funkciya mass, komu interesno, 0.294).


astro-ph/0403710 O mehanizme obrazovaniya malomassivnyh kompaktnyh ob'ektov (On the mechanism of low-mass compact object formation)
Authors: S.B.Popov
Comments: 4 pages

Rech' idet o neitronnyh ili kvarkovyh zvezdah. Vse tochno izvestnye massy etih ob'ektov (izmerennye v dvoinyh pul'sarah) lezhat v intervale ot 1.44 Mo do 1.25 Mo (prichem poslednyaya cifra poyavilas' tol'ko v 2004 godu, a do etogo figurirovala 1.35 Mo). Etot interval primerno sootvetstvuet vozmozhnomu intervalu mass yader massivnyh predsverhnovyh. A kak poluchit' neitronnuyu zvezdu s massoi 1 Mo ili nizhe? Predpolozhenie, vyskazannoe v dannoi stat'e, - fragmentaciya, prichem bol'she, chem na dve chasti, s posleduyushim vybrosom odnogo ili neskol'kih chastei v rezul'tate dinamicheskogo vzaimodeistviya.

(Kazhetsya, eto pervyi sluchai, kogda odin iz avtorov dannyh obzorov, kommentiruet stat'yu drugogo.)


Vypusk 72. 01-15 marta 2004

miniobzor astro-ph/0403038 Neitrinnyi processy v sverhnovyh i neitronnyh zvezdah v ih "mladenchestve" i "starosti" (Neutrino Processes in Supernovae and Neutrons Stars in Their Infancy and Old Age)
Authors: M. Prakash, S. Ratkovic, S. I. Dutta and PALS
Comments: 19 pages, 12 figures

Obsuzhdayutsya neitrinnye processy v poluprozrachnom (dlya neitrino) veshestve sverhnovyh i pochti neprozrachnyh protoneitronnyh zvezdah. Rassmatrivayutsya voprosy registracii neitrinnogo signala na Zemle na sushestvuyushih ustanovkah i vozmozhnost' na etoi osnove razlichit' te ili inye modeli neitronnyh zvezd.

Registraciya neitrinnogo signala ot sverhnovoi 1987A na ustanovkah Kamiokande i IMB byla vozmozhna tol'ko na rannih etapah sushestvovaniya protoneitronnoi zvezdy (<10 s) i ne nakladyvalo ogranichenii na massu i svoistva neitronnoi zvezdy. Registraciya vspyshki sverhnovoi v centre nashei Galaktiki na sovremennyh ustanovkah (SNO, USO ili SuperKamiokande) pozvolit opredelit' massu neitronnoi zvezdy i opredelit' sostoyanie ee veshestva.


astro-ph/0403074 Relyativistskie raschety sliyaniya dvoinyh neitronnyh zvezd (Relativistic Calculations of Coalescing Binary Neutron Stars)
Authors: Joshua Faber, Philippe Grandclement, and Frederic Rasio
Comments: 7 pages

Avtory (uzhe davno izvestnye po rabotam v etoi oblasti) razrabotali novyi, polnost'yu relyativistskii kod dlya modelirovaniya zadachi, privedennoi v nazvanii stat'i. Sledovatel'no, esli testy programmy proidut udovletvoritel'no, cherez nekotoroe vremya nado zhdat' novyh i interesnyh rezul'tatov v dannom napravlenii.


!!! astro-ph/0403076 Priroda zatmenii v dvoinom pul'sare J0737-3039 (Nature of eclipses in binary pulsar J0737-3039)
Authors: Maxim Lyutikov (McGill University, CITA)
Comments: 25 pages, 10 figures. Submitted to MNRAS

U nedavno otkrytogo "dvazhdy dvoinogo" pul'sara J0737-3039 (sm. astro-ph/0312071 i stat'yu na astronet.ru), tochnee u ego molodogo i medlenno vrashayushegosya (2.8 s) komponenta nablyudaetsya strannyi effekt: on izluchaet radioimpul's tol'ko na opredelnennyh orbital'nyh fazah, a v ostal'noe vremya on ne viden.

V dannoi rabote predlozheno vozmozhnoe ob'yasnenie etogo effekta: ono sostoit vo vzaimodeistvii magnitosfery medlennogo pul'sara s relyativistskim vetrom ot millisekundnogo komponenta. Dannuyu ideyu illyustriruyut privedennye nizhe shemy, a za ostal'nymi detalyami pridetsya obrashat'sya k stat'e.


astro-ph/0403170 Ohlazhdenie neitronnyh zvezd. Adronnaya model' (Cooling of Neutron Stars. Hadronic Model)
Authors: D. Blaschke, H. Grigorian, D.N. Voskresensky
Comments: 15 pages, 23 figures

Avtory issleduyut razlichnye effekty, vliyayushie na ohlazhdenie neitronnyh zvezd. Eta pervaya stat'ya iz serii, v nei rassmatrivayutsya adronnye zvezdy, t.e. ob'ekty, ne soderzhashie kvarkovoi materii. V ramkah razumnyh predpolozhenii udaetsya opisat' nablyudaemye ohlazhdayushiesya molodye neitronnye zvezdy.


Vypusk 71. 23-29 fevralya 2004

astro-ph/0402518 Rentgenovskoe izluchenie ot dvoinogo pul'sara J0737-3039 (X-Ray Emission from the Double Pulsar System J0737-3039)
Authors: M. A. McLaughlin et al.
Comments: 5 pages, 4 figures, accepted by ApJ Letters

S pomosh'yu sputnika Chandra udalos' zaregistrirovat' rentgenovskoe izluchenie ot dvoinogo radiopul'sara J0737-3039. Eto pervyi sluchai registracii rentgena ot dvoinoi neitronnoi zvezdy. Izluchenie neteplovoe. Dannye soglasuyutsya s model'yu, v kotoroi za rentgen otvetstvena magnitosfera bolee energichnogo pul'sara J0737-3039A.


Vypusk 70. 16-22 fevralya 2004

astro-ph/0402349 CFL zvezdy v dvoinyh sistemah: "pryachutsya" li oni sredi kandidatov v chernye dyry? (Self-bound CFL stars in binary systems : are they "hidden" among the black hole candidates?)
Authors: J. E. Horvath, G. Lugones
Comments: 4 pages, 3 figures

My neodnokratno obrashali vashe vnimanie na raboty, posvyashennye probleme "identifikacii" chernyh dyr (Narayan et al.; Abramowicz et al.). Osobo hochetsya vydelit' nedavnyuyu stat'yu Ye-Fei Yuan et al.. Problema v obnaruzhenii neposredstvennogo proyavleniya gorizonta.

Narayan et al. polagayut, chto lyuboi kompaktnyi ob'ekt s massoi bolee 3 mass solnca i bez rentgenovskih vspleskov pervogo tipa (oni svyazany s zagoraniem "termoyadernogo topliva" na poverhnosti) yavlyaetsya ochen' sil'nym kandidatom v chernye dyry. Horvat i Lugones v svoei stat'e rassmatrivayut nekotoruyu ekzoticheskuyu al'ternativu - CFL zvezdy (CFL=color flavor locked).

CFL zvezdy eto podvid togo, chto inogda ob'edinyayut obshim terminom "neitronnye zvezdy". Na samom dele v zavisimosti ot uravneniya sostoyaniya sostav kompaktnogo ob'ekta mozhet byt' sovsem ne "neitronnym". V chastnosti, mogut sushestvovat' kvarkovye zvezdy raznyh tipov. CFL zvezdy - odin iz nih. Eti ob'ekty otlichayutsya dovol'no bol'shimi maksimal'nymi massami i otsutstviem normal'noi poverhnosti. T.o. po mneniyu avotrov oni mogut pryatat'sya sredi kandidatov v chernye dyry "po Narayanu".

Stat'ya korotkaya i ponyatnaya. Tak chto v nei legko razobrat'sya.


astro-ph/0402392 Evolyuciya magnitnogo polya v kore neitronnyh zvezd pod deistviem effekta Holla i omicheskogo zatuhaniya (Magnetic Field Evolution in Neutron Star Crusts due to the Hall Effect and Ohmic Decay)
Authors: Andrew Cumming et al.
Comments: 18 pages, 13 figures, Submitted to ApJ

Eshe odna stat'ya pro evolyuciyu magnitnogo polya u neitronnyh zvezd. Ee osobennost' - uchet effekta Holla (naryadu s drugimi effektami). Privedeny rezul'taty chislennogo modelirovaniya, pokazany vozmozhnye konfiguracii polei.

[Effekt Holla zaklyuchaetsya v vozniknovenii v provodnike s tokom I, pomeshennom v magnitnoe pole B, elektricheskogo polya v napravlenii, perpendikulyarnom k I i B. Svyazan s otkloneniem dvizhushihsya v provodnike elektronov silami Lorenca.]


obzor astro-ph/0402404 Dekonfaiment kvarkov i ego vliyanie na radiusy i predel'nye massy kompaktnyh zvezd (Quark deconfinement and implications for the radius and the limiting mass of compact stars)
Authors: Ignazio Bombaci et al
Comments: 34 pages, 10 figures

Avtory yavlyayutsya storonnikami shiroko rasprostranennoi segodnya gipotezy, chto v kompaktnyh (neitronnyh) zvezdah vozmozhen perehod ot nuklonnogo veshestva k kvarkovoi plazme, no v otlichie ot bol'shinstva issledovatelei oni priderzhivayutsya mneniya, chto takoi perehod budet proishodit' postepenno i zvezda mozhet nadolgo zaderzhat'sya v metastabil'nom "gibridnom" perehodnom sostoyanii.

Avtory podrobno rassmatrivayut svoi variant teorii, razlichnye ego sledstviya i, v chastnosti, ee prilozhenie k "zaderzhannym" gamma-vspleskam, kotorye proishodyat cherez nekotoroe vremya posle kollapsa massivnoi zvezdy.


!!! astro-ph/0402418 Sil'naya shirokaya liniya poglosheniya v rentgenovskom spektre blizkoi odinochnoi neitronnoi zvezdy RX J1605.3+3249 (A Strong, Broad Absorption Feature in the X-ray Spectrum of the Nearby Neutron Star RX J1605.3+3249)
Authors: M. H. van Kerkwijk et al.
Comments: 30 pages, 7 figures, accepted in ApJ

Nablyudeniya observatorii XMM-N'yuton pokazali, chto v spektre tret'ei po yarkosti odinochnoi neitronnoi zvezdy nablyudaetsya shirokaya i moshnaya absorbcionnaya osobennost' (proshe govorya, liniya poglosheniya). Centr etoi linii prihoditsya na Dlinu volny 27 angstrem ili na energiyu 0.45 keV. V stat'e podrobno opisana metodika provedeniya i obrabotki nablyudenii, no osnovnoe mozhno pocherpnut' iz privedennogo nizhe risunka.


Srektr ob'ekta RX J1605.3+3249, sploshnoi i punktirnoi liniyami pokazany kontinuumy dvuh naibolee udachnyh ego approksimacii (bez ucheta linii poglosheniya).

Avtory prihodyat k zaklyucheniyu, chto eto protonnaya ciklotronnaya liniya, oslablennaya kvantovymi vakuumnymi effektami. V etom sluchae magnitnoe pole na poverhnosti dolzhno bylo by sostavlyat' 7x1013 Gs (bez ucheta gravitacionnogo pokrasneniya).


Vypusk 69. 08-15 fevralya 2004

obzor astro-ph/0402136 Odinochnye neitronnye zvezdy (Isolated Neutron Stars)
Authors: V. M. Kaspi, M. S. E. Roberts, A. K. Harding
Comments: 66 pages, 17 figures. To appear in "Compact Stellar X-ray Sources", eds. W.H.G. Lewin and M. van der Klis. Comments welcome but needed ASAP. High resolution images and Tables 8.1 and 8.2 available at http://www.physics.mcgill.ca/~vkaspi/isolated_neutron_stars

Odnovremenno poyavilis' dva obzora po neitronnym zvezdam: etot i obzor Yakovleva i Petika po ohlazhdeniyu. V etom obzore daetsya svod dannyh po rentgenovskomu izlucheniyu ot odinochnyh neitronnyh zvezd. Ono mozhet byt' svyazano ili s vrasheniem (kak u pul'sarov), ili s vysokoi temperaturoi. Sootvetstvenno opisyvayutsya kak dannye nablyudenii, tak i teorii.


obzor astro-ph/0402143 Ohlazhdenie neitronnyh zvezd (Neutron Star Cooling)
Authors: D.G. Yakovlev, C.J. Pethick
Comments: 41 pages, 12 figures, to appear in Ann. Rev. Astron. Astrophys., 2004

Obzor prekrasno dopolnyaet vysheopisannyi material Kaspi i dr. Zdes' detal'no opisyvaetsya ohlazhdenie neitronnyh zvezd. Dannye o temperature takih ob'ektov v osnovnom poluchayutsya kak raz iz rentgenovskih nablyudenii. Tak chto obzory otlichno stykuyutsya drug s drugom.


miniobzor astro-ph/0402175 Istochniki myagkih povtoryayushihsya gamma-vspleskov i anomal'nye rentgenovskie pul'sary: naveki vmeste (Soft Gamma Repeaters and Anomalous X-ray Pulsars: Together Forever)
Authors: V. M. Kaspi
Comments: 8 pages, 2 figures. To appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler

Odnovremenno poyavilis' srazu dva obzora po anomal'nym rentgenovskim pul'saram (ARP) i istochnikam myagkih povtoryayushihsya gamma-vspleskov (MPG). Vtoraya stat'ya (Anomalous) X-ray Pulsars posvyashena, kak yasno iz nazvaniya, v osnovnom ARP. V etoi zhe daetsya svodka po oboim tipam ob'ektov. Obsuzhdayutsya vzaimosvyazi mezhdu ARP i MPG (cherez vspyshki i drugie proyavleniya).

Osnovnoi vyvod Viki Kaspi takov: magnetarnaya gipoteza yavlyaetsya samoi sil'noi na segodnyashnii den', odnako, somneniya ostayutsya, a potomu nuzhny bolee detal'nye i pryamye nablyudeniya.


miniobzor astro-ph/0402200 Obrazovanie neitronnyh zvezd i ih nachal'nye svoistva (Neutron Star Formation and Birth Properties)
Authors: Hans-Thomas Janka
Comments: 10 pages, 4 figures, high-quality available upon request; to appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds. F. Camilo and B.M. Gaensler

Horoshii ochen' dostupnyi obzor, posvyashennyi obrazovaniyu neitronnyh zvezd. Obsuzhdayutsya naibolee standartnye vzglyady na nachal'nye svoistva etih ob'ektov: massy, periody, skorosti, magnitnye polya i t.p.


astro-ph/0402231 1E1207.4-5209 unikal'nyi ob'ekt (1E1207.4-5209 - a Unique Object)
Authors: G.F. Bignami et al.
Comments: 6 pages, 6 figures

Unikal'naya odinochnaya neitronnaya zvezda v rentgenovskom spektre kotoroi nablyudayutsya shirokie i glubokie linii. My o nei uzhe pisali god nazad (sm. astro-ph/0301161). Za god intensivnyh nablyudenii poluchen ryad interesnyh rezul'tatov, kotorye korotko izlozheny v etoi nebol'shoi zametke.


astro-ph/0402232 Geminga: rasskaz o dvuh hvostah i bolee togo (Geminga: a tale of two tails, and much more)
Authors: P.A. Caraveo, et al.
Comments: 6 pages, 4 figures

V zametke kratko izlozhen rezul'taty glubokogo (bolee sutok) nablyudeniya pul'sara Geminga s borta observatorii XMM-N'yuton. Na izobrazhenii yasno vidny dva parallel'nyh napravleniyu dvizheniya pul'sara "hvosta", vyzvannyh ego vzaimodeistviem s mezhzvezdnoi sredoi. Eto samaya interesnaya kartinka (sm. nizhe), ostal'nye "vkusnosti" otnosyatsya k spektru etogo pul'sara.


astro-ph/0402282 Dvizhenie pul'sarov v Galaktike (Pulsar motions in our Galaxy)
Authors: X. H. Sun, J. L. Han
Comments: 11 pages, 16 figures, accepted by MNRAS

S pomosh'yu chislennogo modelirovanie otslezhivayutsya orbity radiopul'sarov v Galaktike v techenie pervyh 2 milliardov let ih zhizni. Takie raboty uzhe neodnokratno provodilis' (v tom chisle i nami), odnako poyavlyayutsya novye dannye, utochnyayutsya razlichnye parametry, poetomu povtorenie takih issledovanii neobhodimo.


Vypusk 68. 01-07 fevralya 2004

miniobzor astro-ph/0402013 Vysokochastotnye QPO kak fizicheskaya problema: nelineinyi rezonans (High-frequency QPOs as a problem in physics: non-linear resonance)
Authors: Wlodek Kluzniak, Marek A. Abramowicz, William H. Lee
Comments: 4 pages, presented at X-ray Timing 2003: Rossi and Beyond, Boston, November 2003

QPO - kvaziperiodicheskie oscillyacii. Eto vazhnyi fenomen, nablyudayushiisya v akkreciruyushih tesnyh dvoinyh sistemah s neitronnymi zvezdami i chernymi dyrami. Prichiny vozniknoveniya QPO neyasny. Est' dostatochno mnogo modelei i vse vremya poyavlyayutsya novye (sm. samuyu poslednyuyu v svezhei rabote The MHD Alfven wave oscillation model of kHz Quasi Periodic Oscillation of Accreting X-ray Binaries).

Zdes' zhe avtory rassmatrivayut QPO kak nelineinyi rezonans (sm. takzhe ih stat'yu Resonance in forced oscillations of an accretion disk and kHz QPOs). Poskol'ku yavlenie nablyudaetsya i u sistem s neitronnymi zvezdami, i u sistem s chernymi dyrami, to, polagayut avtory, nado smotret' na to obshee, chto u nih est'. U chernyh dyr net ni poverhnosti, ni magnitnogo polya. Znachit, ostaetsya akkrecionnyi disk. I imenno on igraet klyuchevuyu rol' v ih modeli: QPO - eto rezonansnye kolebaniya akkrecionnogo diska.

V otdel'noi stat'e (astro-ph/0402012) avtory rassmatrivayut QPO v sistemah s chernymi dyrami, nadeyas' s pomosh'yu etogo instrumenta poluchit' otvet o prirode ul'tramoshnyh rentgenovskih istochnikov.


astro-ph/0402122 Ot modeli Skirma k gipoteticheskim skirmionym zvezdam (From the Skyrme model to hypothetical Skyrmion stars: Astrophysical implications)
Authors: Rachid Ouyed
Comments: 8 pages, 1 figure. Submitted to New Astronomy

Poskol'ku tochnoe povedenie veshestva pri vysokoi plotnosti neizvestno, ot teoretiki prodolzhayut razrabatyvat' razlichnye modeli. Dlya proverki etih postroenii mozhno ispol'zovat' kompaktnye ostatki evolyucii massivnyh zvezd - to, chto my nazyvaem "neitronnye zvezdy".

V 60-e gg. Skirm (T. Skyrme) sozdal teoriyu pionnogo vzaimodeistviya. Etu model' inogda nazyvayut solitonnoi: bariony v nei yavlyayutsya topologicheskimi solitonami (imenno na osnove etoi modeli D'yakonov, Petrov i Polyakov predskazali v 1997 g. pentakvarki, sm. takzhe hep-ph/0009006 i bolee populyarnye materialy).

Zdes' zhe avtor pytaetsya posmotret' kakie kompakntyne ob'ekty mozhno sozdat' na osnove modeli Skirma. Osnovnoe svoistvo takih skirmionnyh zvezd - bol'shaya massa (okolo 2 mass Solnca i dazhe chut' bol'she). Radius u takih ob'ektov tozhe chut' bol'she, chem u standartnoi neitronnoi zvezdy - okolo 15-16 km. Sredi neitronnyh zvezd izvestny ob'ekty s massoi bolee dvuh mass Solnca (naprimer, Vela X-1). Tak chto model' predstavlyaet interes. Verna li ona pokazhet budushee.


Vypusk 67. 26-31 yanvarya 2004

astro-ph/0401476 Glitch akkreciruyushego pul'sara (A Frequency Glitch in an Accreting Pulsar)
Authors: D.K. Galloway et al.
Comments: 10 pages, 4 figures; submitted to ApJ

Glitch - eto sboi perioda vrasheniya. Nablyudayutsya oni u obychnyh radiopul'sarov (naprimer, u pul'sara v Krabe) i nedavno byli otkryty u anomal'nyh rengenovskih pul'sarov. No nikogda glitchi ne nablyudalis' u akkreciruyushih neitronnyh zvezd v tesnyh dvoinyh sistemah.

Pri glitche skachkom menyaetsya period vrasheniya. Menyaetsya na neznachitel'nuyu velichinu. Svyazyvayut eto ili s izmeneniem momenta inercii kory zvezdy, ili s otryvom vihrevyh nitei, kotorye "pricepleny" k kore iznutri.

Avtory etoi raboty privodyat dannye o rezkom (zavedomo menee 10 chasov) izmenenii perioda neitronnoi zvezdy v sisteme KS 1947+300. Eto dvoinaya s Ve-zvezdoi. Period vrasheniya neitronnoi zvezdy 18.7 sekundy. Vvidu slozhnosti povedeniya perioda vrasheniya akkreciruyushih neitronnyh zvezd v dvoinyh sistemah avtory rassmatrivayut razlichnye prichiny skachka perioda. Odnako, po ih mneniyu, glitch - samaya veroyatnaya. Tem ne menee otmetim, chto delo eto poka temnoe. Tem bolee, chto glitch poluchaetsya ochen' netipichnym kak po velichine, tak i po posleduyushei evolyucii vrasheniya neitronnoi zvezdy. V lyubom sluchae, avtoram udalos' uvidet' ochen' interesnoe yavlenie.


astro-ph/0401553 K voprosu o nizkoi masse kompan'ona v sisteme J0737-3039 (On the Low Progenitor Mass of the Binary Pulsar J0737-3039B)
Authors: Tsvi Piran, Nir J. Shaviv
Comments: 12 pages, 3 figure

Kak navernoe mnogie pomnyat, v nedavno otkrytoi sisteme, sostoyashei iz dvuh radiopul'sarov, massa vtorogo komponenta dovol'no mala - okolo 1.25 massy Solnca. Avtory rassuzhdayut o tom, s chem eto mozhet byt' svyazano.

Problema kroetsya v tom, chto esli sistema bystro sbrasyvaet bolee poloviny massy, to ona razrushaetsya (eto esli net special'no podobrannoi skorosti otdachi pri sbrose). Pri mnogih "podgonochnyh" variantah s sohraneniem sistemy poluchaetsya dovol'no bol'shoi ekscentrisitet, a u J0737-3039 on kak raz mal (menee 0.1). Krome togo, sistema sidit blizko ot ploskosti Galaktiki, chto yavlyaetsya argumentom v pol'zu maloi skorosti otdachi. Znachit, poluchaetsya, chto bylo sbrosheno ochen' malo veshestva pri pochti nulevoi otdache. Massa predsverhnovoi poluchaetsya menee 2 mass Solnca (dazhe vozmozhno menee 1.5). Voobshe govorya, eto ne ochen' horosho soglasuetsya s teoriyami vzryvov sverhnovyh ....


astro-ph/0401555 Tormozhenie magnitara, gipermoshnye sverhnovye i gamma-vspleski (Magnetar Spindown, Hyper-Energetic Supernovae, and Gamma Ray Bursts)
Authors: Todd A. Thompson et al.
Comments: 16 pages, 5 figures, emulateapj

V stat'e avtory pytayutsya uvyazat' v edinoe celoe formirovanie sil'nozamagnichennyh neitronnyh zvezd (magnitarov), gamma-vspleski i sverhnovye s bol'shim energovydeleniem. Sut' sostoit v tom, chto esli obrazuetsya bystrovrashayushayasya sil'nozamagnichennaya neitronnaya zvezda, to dinamika povedeniya udarnoi volny budet sil'no drugoi. Eto mozhet kak dat' dopolnitel'nuyu energiyu dlya vzryva, tak i sozdat' usloviya dlya gamma-vspleska (dzhety, naprimer).

O magnitarah mozhno takzhe prochest' v rabote astro-ph/0401561.


nucl-th/0401052 Vliyanie cvetnoi sverhprovodimosti na strukturu i obrazovanie kompaktnyh ob'ektov (Effects of color superconductivity on the structure and formation of compact stars)
Authors: Drago, A. et al.
Comments: 4 pages, 2 figures. To be published in Phys.Rev.D

Uzhe davno obsuzhdaetsya vozmozhnost' sushestvovaniya razlichnyh ekzoticheskih sostoyanii materii v nedrah togo, chto my nazyvaem "neitronnye zvezdy". Soglasno ryadu modelei mnogie iz nih iz neitronov i ne sostoyat! Inogda vydelyayut takie chetyre gruppy:
I. Adronnye zvezdy (v nih ne proizoshel t.n. dekonfainment - vysvobozhdenie kvarkov)
1. Obychnye neitronnye zvezdy. Sostoyat celikom iz obychnoi yadernoi materii.
2. Giperonnye zvezdy. V nedrah est' giperony.
II. Kvarkovye zvezdy.
1. Gibridnye zvezdy. V nih est' kvarkovoe yadro i normal'naya vneshnyaya chast'.
2. "Golye" (bare) kvarkovye zvezdy. Net dazhe vneshnei kory (ili ona ochen'-ochen' tonkaya).

V poslednee vremya aktivno stali obsuzhdat' astrofizicheskie proyavleniya dopolnitel'nogo energovydeleniya, svyazannogo s dekonfainmentom. A tam est' chto obsuzhdat'! Energii - kak u sverhnovoi. Sootvetstvenno rassmatrivayut dva varianta: vydelenie energii srazu posle obrazovaniya kompaktnogo ob'ekta ili zhe zaderzhka (otlozhennyi dekonfainment). V pervom sluchae daetsya dopolnitel'nyi vklad v dinamiku vzryva. Vo vtorom - mozhno sdelat' gamma-vsplesk cherez nekotoroe vremya posle vzryva sverhnovoi. Obe vozmozhnosti ochen' interesny i ochen' vazhny, t.k. pomogayut ob'yasnyat' real'nye nablyudeniya.

Sobstvenno, v samoi stat'e ne predlagaetsya nichego revolyucionnogo. Avtory rassmatrivayut nekotorye detali modelei. No ona budet bezuslovno interesna tem, kto eshe nichego po etoi teme ne chital (hotya speshim zametit', chto stat'ya ne rasschitana na populyarnoe izlozhenie).


Vypusk 66. 19-26 yanvarya 2004

astro-ph/0401334 Tochnoe polozhenie anomal'nogo rentgenovskogo pul'sara XTE J1810-197 i ego identifikaciya v IK (Accurate X-ray position of the Anomalous X-ray Pulsar XTE J1810-197 and identification of its likely IR counterpart)
Authors: G.L. Israel et al.
Comments: 5 pages, 2 figures. Accepted for publication on ApJ Letters

Napomnim, chto anomal'nye rentgenovskie pul'sary byli vydeleny v otdel'nyi klass na osnove blizosti periodov (5-10 sekund), otsutstviya vtorogo komponenta i stabil'nogo zamedleniya vrasheniya (uvelicheniya perioda). Naibolee populyarnoi gipotezoi o prirode etih istochnikov yavlyaetsya magnitarnaya teoriya Tompsona i Dunkana (krome togo, ryad avtorov prodolzhaet razvivat' teoriyu akkrecii iz ostatochnogo diska).

V stat'e opisyvayutsya nablyudeniya novogo kandidata v anomal'nye pul'sary. Izyuminka sostoit v sil'noi peremennosti izlucheniya. Problem tut poyavlyaetsya dve. Pervaya sostoit v tom, chto magnitarnaya gipoteza ne predskazyvala takogo povedeniya. Vtoraya takova, koli ob'ekt provodit mnogo vremeni v "tihom" sostoyanii, to chislo takih istochnikov mozhet byt' ochen' veliko.

Chto zh, voprosy zadany - budem dumat' ....


astro-ph/0401375 Trehmernoe modelirovanie diskovoi akkrecii na naklonnyi dipol' (Three-dimensional Simulations of Disk Accretion to an Inclined Dipole: I. Magnetospheric Flow at Different Theta)
Authors: M.M.Romanova et al.
Comments: 26 pages, 22 figures, ApJ, 595 (2003), 1009-1031

Eto ne pervaya rabota dannyh avtorov po chislennoi MGD, do etogo byla akkreciya na soosnyi dipol', na bystro dvizhushuyusya, no nevrashayushuyusya zvezdu i t.d.

Stat'yu mozhno chitat' dvumya sposobami: vnimatel'no vchityvat'sya v ispol'zovannye granichnye usloviya i parametry sredy - eto dlya specialistov gidrodinamikov, fizikov plazmy i astrofizikov, ili prosto smotret' na kartinki - ih mnogo i nizhe privedena odna iz samyh prostyh i ne krasochnyh.


Shema nachal'nyh uslovii rascheta:
sechenie vdol' osi vrasheniya

Na saite avtorov mozhno posmotret' fil'm, sledannyi po etim raschetam: http://www.astro.cornell.edu/us-rus/inclined.htm.


miniobzor astro-ph/0401415 Triggery vspleskov magnitarov (Triggers of magnetar outbursts)
Authors: Robert C. Duncan
Comments: Invited review, "3-D Signatures in Stellar Explosions," eds. P.Hoeflich, P. Kumar & J.C. Wheeler (Cambridge Univ. Press 2004) [15 pages, no figures]

V naibolee populyarnoi i prorabotannoi modeli istochniki myagkih povtoryayushihsya gamma-vspleskov (MPG) i anomal'nye rentgenovskie pul'sary (ARP) yavlyayutsya sil'nozamagnichennymi neitronnymi zvezdami - magnitarami. Vremya ot vremeni na nih proishodyat vspyshki. Est' teoriya, chto vspyshki svyazany s peresoedineniem magnitnyh silovyh linii. Peresoedinenie linii mozhet byt' svyazano s neustoichivostyami v magnitosfere, a mozhet - s podvizhkami kory. V dannoi stat'e avtor razvivaet vtoruyu ideyu.

V nachale daetsya kratkoe vvedenie. Tam opisyvaetsya (na kachestvennom urovne) stroenie vneshnih sloev neitronnoi zvezdy (vy uznaete, chto takoe "yadernye spagetti", "yadernaya lazan'ya" i "invertirovannye belyashi"). Kstati, v zemnyh laboratoriyah uchenye uspeshno izuchayut sostoyanie veshestva, kachestvenno pohozhee na koru neitronnoi zvezdy. Zatem opisyvaetsya nablyudatel'naya storona dela. Nakonec vo vtoroi polovine raboty Dunkan rasskazyvaet, kak processy v kore neitronnoi zvezdy mogut privodit' k vspyshkam.


astro-ph/0401472 Rentgenovskii pul'sar, bogatyi metallami vybros i udarnaya volna v okruzhayushem veshestve v ostatke sverhnovoi G292.0+1.8 (An X-Ray Pulsar, Metal-rich Ejecta, and Shocked Ambient Medium in the Supernova Remnant G292.0+1.8)
Authors: John P. Hughes et al.
Comments: 4 pages, including 3 postscript figs, LaTeX, to appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler

Poskol'ku neitronnye zvezdy otnosyatsya k nashei oblasti professional'nyh interesov, to my pishem o nih dostatochno chasto. Takzhe my ne ustaem povtoryat', chto s nachal'nymi parametrami neitronnyh zvezd daleko ne vse yasno. Yasno tol'ko, chto rozhdayutsya oni ochen' raznymi. Poetomu privlekayut vnimanie istochniki v ostatkah sverhnovyh ...

Ostatok G292.0+1.8 schitaetsya ochen' pohozhim na Cas A, gde pervye zhe nablyudeniya Chandry vyyavili ochen' strannyi tochechnyi istochnik. Do sih por neyasno yavlyaetsya li on neitronnoi zvezdoi ili chernoi dyroi, no uzh tochno ne yavlyaetsya normal'nym molodym radiopul'sarom (tipa Kraba).

V G292.0+1.8 uzhe byla izvestna pul'sarnaya tumannost', a potom byl obnaruzhen i radiopul'sar s periodom 0.135 sekundy. I vot po dannym Chandra udalos' uvidet' pul'sacii i v rentgene. V optike na meste radiopul'sara nichego ne vidno vplot' do 26-i zvezdnoi velichiny.


Vypusk 64. 01-11 yanvarya 2004

superotkrytie!!! astro-ph/0401086 Dvuh pul'sarnaya sistemy - redkaya udacha dlya relyativistskoi fiziki i fiziki plazmy (A Double-Pulsar System - A Rare Laboratory for Relativistic Gravity and Plasma Physics)
Authors: A.G.Lyne et al.
Comments: 21 pages, 5 figures, Science, in press

Nastupil moment, kotorogo tak zhdali! Otkryta sistema iz dvuh neitronnyh zvezd, kazhdyi komponent kotoroi yavlyaetsya radiopul'sarom! Etoi dolgozhdannoi sistemoi okazalsya nedavno otkrytyi, samyi tesnyi iz izvestnyh, dvoinoi pul'sar J0737-3039. Teper' odnu ego komponentu s periodom 22 ms budut nazyvat' J0737-3039A, a druguyu, s periodom 2.8 s, J0737-3039B. Eta sistema horosha eshe tem, chto imeet ochen' korotkii orbital'nyi period (2.4 ch) i nablyudaetsya pochti s rebra (naklonenie orbity okolo 87o).

Obnaruzhenie dannoi sistemy otkryvaet velikolepnye perspektivy dlya dal'neishei proverki OTO, dlya pryamogo izucheniya magnitosfer pul'sarov i dlya issledovaniya svoistv neitronnyh zvezd. Etot pul'sar pahnet nobelevskoi premiei, vozmozhno dazhe ne odnoi. Podrobnee o ego svoistvah mozhno prochitat' v etoi zametkah na Astronete i Pereplete.


astro-ph/0401119 Novye pul'sary vblizi neotozhdestvlennyh gamma-istochnikov (New Pulsars Coincident With Unidentified Gamma-Ray Sources)
Authors: Mallory S.E. Roberts et al.
Comments: 4 pages, 1 table
astro-ph/0401120 Novye poiski pul'sarov v boksah oshibok neotozhdestvlennyh istochnikov EGRET (Recent Searches for Pulsars in Unidentified EGRET Error Boxes)
Authors: Mallory S.E. Roberts
Comments: 6 pages, 1 figure

Bol'shaya chast' iz primerno 300 gamma-istochnikov v kataloge, sozdannom v eksperimente EGRET, do sih por ostaetsya neotozhdestvlennoi. Vblizi 56 takih istochnikov lezhashih ne tochno v ploskosti Galaktiki (|b|>5o) i ne sovpadayushih s izvestnymi blazarami, na rabioobservatorii Parks v Avstralii byl proveden poisk radiopul'sarov. V rezul'tate dannogo obzora byli naideny neskol'ko novyh radiopul'sarov, vklyuchaya tri dvoinyh sistemy.


Vypusk 63. 16-31 dekabrya 2003

astro-ph/0312356 Otkrytie pekulyarnogo pul'sara v Malom Magellanovom Oblake (A Discovery of a Peculiar Pulsar in the Small Magellanic Cloud)
Authors: Masaru Ueno et al.
Comments: 5 pages, 5 figures, accepted in PASJ

V stat'e opisyvayutsya ochen' neobychnye svoistva rentgenovskogo pul'sara s Be-zvezdoi IKT1 (=RXJ0047.3-7312) po dannym nablyudenii, provedennyh orbital'noi observatoriei XMM-N'yuton v oktyabre 2000 g. U pul'sara nablyudayutsya sushestvennye izmeneniya potoka s periodom okolo 4000 s i kogerentnye pul'sacii s periodom 263+/-1 s. V hode nablyudenii potok sushestvenno menyalsya, ego srednee znachenie v intervale energii 0.7-10 keV sostavlyalo 2.9x10-12 erg/sm2/s, chto primerno v 10 raz bol'she, chem pri nablyudeniyah s ROSAT a v 1999 g. Vse pekulyarnye svoistva nablyudalis' tol'ko v myagkoi spektral'noi komponente izlucheniya (T=0.6 keV) i ne zatragivali zhestkuyu (s T=5.8 keV).


obzor astro-ph/0312369 Odinochnye neitronnye zvezdy: astrofizicheskii obzor (Isolated neutron stars: An astrophysical perspective)
Authors: Sergei Popov, Roberto Turolla
Comments: 20 pages, 6 figures, Review talk given at the NATO Advanced Research Workshop On Superdense QCD Matter and Compact Stars, 27 Sep - 4 Oct 2003, Yerevan, Armenia

Eto obzornyi doklad, prochitannyi na, v obshem-to, fizicheskoi konferencii po kvarkovym zvezdam i ekstremal'nym sostoyaniyam veshestva.

V pervoi chasti daetsya spisok naibolee interesnyh rezul'tatov, poluchennyh za poslednie 2-3 goda. Zatem dayutsya bolee podrobnye kommentarii po spektram i atmosferam neitronnyh zvezd, po akkrecii na odinochnye neitronnye zvezdy, i po nekotorym drugim voprosam, predstavlyayushim interes dlya avtorov obzora.


astro-ph/0312399 Dlinnye i korotkie gamma-vspleski i otdacha pul'sarov (Long and short gamma-ray bursts, and the pulsar kicks)
Authors: Alexander Kusenko and Dmitry V. Semikoz
Comments: 8 pages, 1 figure

Ideya raboty ochen' ponyatna: korotkie gamma vspleski ochen' pohozhi na pervye neskol'ko sekund dlinnyh gamma-vspleskov, kotorye po kakoi-to prichine vnezapno zakonchilis'. Avtory predpolagayut, chto eto imenno tak. Gamma-vspleski porozhdayutsya v hode sverhmoshnoi akkrecii veshestva iz akkrecionnogo diska (obrazovavshegosya iz obolochek kollapsiruyushei zvezdy) na neitronnuyu zvezdu ili chernuyu dyru. Poka idet akkreciya my nablyudaem gamma-izluchenie. No esli za neskol'ko sekund neitronnaya zvezda priobretaet vysokuyu skorost', to ona mozhet vyletet' iz diska i vsplesk prekratitsya.


astro-ph/0312413 Zavisyashaya ot fazy liniya poglosheniya v spektre rentgenovskogo pul'sara RX J0720.4-3125 (A phase-dependent absorption line in the spectrum of the X-ray pulsar RX J0720.4-3125)
Authors: F. Haberl et al.
Comments: 9 pages, 10 figures, Submitted to A&A

V spektre odinochnoi neitronnoi zvezd RX J0720.4-3125 observatoriya XMM-N'yuton obnaruzhila spektral'nuyu liniyu s energiei 400 eV Shirina i polozhenie linii menyayutsya sinhronno s fazoi vrasheniya neitronnoi zvezdy. Iz etih dannyh poluchaetsya ocenka magnitnogo polya 5x1013 Gs. Ocenka soglasuetsya s dannymi po tormozheniyu vrasheniya pul'sara.


miniobzor! astro-ph/0312542 Skorosti neitronnyh zvezd i asimmetriya vzryva sverhnovoi (Neutron Star Kicks and Supernova Asymmetry)
Authors: Dong Lai
Comments: 11 pages, to appear in 3D Signatures of Stellar Explosion, a workshop honoring J.C. Wheeler's 60th Birthday

Odnim iz vazhneishih svoistv neitronnyh zvezd yavlyayutsya ih nachal'nye skorosti, t.k. po vsei vidimosti oni nesut na sebe otpechatok vzryva sverhnovoi. Pri vzryve vydelyaetsya kolossal'naya energiya - 1053 erg (1046 Dzh). Bol'shaya ee chast' unositsya neitrino. Ostal'noe izluchaetsya v vide elektromagnitnogo i gravitacionnogo izlucheniya, a takzhe perehodit v mehanicheskuyu energiyu sbroshennogo veshestva. Dazhe esli dopustit' nebol'shuyu (poryadka procenta) asimmetriyu vzryva, to obrazovavshiisya kompaktnyi ostatok poluchit' kik (tolchok), v rezul'tate chego my budem potom nablyudat', naprimer, bystro dvigayushiisya pul'sar. Izmerennye skorosti etih ob'ektov dostigayut 2000 km/s !!!

Avtor daet obzor osnovnyh mehanizmov poyavleniya kika:
Gidrodinamicheskii,
Neitrinnyi,
Elektromagnitnyi.

Ukazhem takzhe na lyubopytnuyu vozmozhnost' togo, chto naibolee bystrodvigayushiesya kompaktnye ob'ekty - eto kvarkovye zvezdy.


Vypusk 62. 01-15 dekabrya 2003

astro-ph/0312034 Rentgenovskie pul'sary v massivnyh dvoinyh Malogo Magellanovogo Oblaka (High Mass X-ray Binary Pulsars in the Small Magellanic Cloud)
Authors: W.A. Majid, R.C. Lamb, D.J. Macomb
Comments: 26 pages, 10 figures, submitted to ApJ

V rabote soobshaetsya ob otkrytii novogo rentgenovskogo pul'sara s periodom 202 s i podtverzhdaetsya obnaruzhenie nedavno otkrytogo pul'sara s periodom 263 s v Malom Magellanovom Oblake (MMO). Oba istochnika otozhdestvleny s ochen' molodymi B-zvezdami, t.e. vhodyat v massivnye dvoinye sistemy. V nastoyashee vremya v MMO izvestnyi 24 rentgenovskih pul'sara iz kotoryh 14 ostayutsya neotozhdestvlennymi v optike.

Eshe odin rezul'tat dannoi raboty - novoe znachenie predpolagaemogo perioda anomal'nogo rentgenovskogo pul'sara AXP CXOU J010043.1-721134 ravnoe 8.0 s (ranee eta zhe nablyudatel'naya gruppa davala znachenie perioda 5.4 c).


astro-ph/0312044 Parallaksy pul'sarov po nablyudeniyam VLBA na 5 GGc (Pulsar Parallaxes at 5 GHz with the Very Long Baseline Array)
Authors: S.Chatterjee et al.
Comments: 8 pages, 3 figures, 3 tables; submitted to ApJ

Rasstoyanie do pul'sarov - samaya ser'eznaya problema dannoi oblasti nablyudatel'noi astrofiziki, dlya bol'shinstva iz nih rasstoyanie meryaetsya po mere dispersii i imeet nizkuyu tochnost'. Poetomu izmerenie rasstoyanii do pul'sarov lyubym drugim, osobenno pryamym sposobom, ochen' vazhno i interesno.

V dannoi rabote opublikovany izmereniya parallaksov samyh blizkih i samyh yarkih pul'sarov na seti antenn VLBA (Very Long Baseline Array) v SShA na chastote 5 GGc. Parallaksy izmeryalis' dlya pul'sarov B0329+54, B0355+54 i B1929+10, dlya niz bylo provedeno 7 serii nablyudenii, razdelennyh periodom v 2 goda (t.e. ih nablyudeniya dlilis' 12 let). Dlya pul'sara B0329+54 iz-za bol'shih sistematicheskih oshibok poluchena tol'ko verhnyaya ocenka pi<1.5x10-3 ". Dlya dvuh drugih pul'sarov izmereny parallaksy i sobstvennye dvizheniya. Dlya B0355+54 pi=(0.91+/-0.16)x10-3 " (d=1.04+0.21-0.16 KPK), a poperechnaya skorost' - 61 km/s. Dlya pul'sara B1929+10 polucheny znacheniya pi=(2.77+/-0.07)x10-3 " (d=361+/-8 pk), a poperechnaya skorost' - 177+/-5 km/s.


astro-ph/0312071 Uvelichenie ocenki chastoty sliyaniya dvoinyh neitronnyh zvezd po nablyudeniyami sistemy s bol'shimi relyativistskimi effektami (An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system)
Authors: M. Burgay et al.
Comments: 6 pages, 2 figures

Otkryta eshe odna dvoinaya neitronnaya zvezda - samaya tesnaya ih izvestnyh segodnya. Orbital'nyi period etoi sistemy vsego 2.4 chasa i ona sol'etsya cherez 85 millionov let. Otkrytie etoi dvoinoi pochti v desyat' raz povysilo ozhidaemyi temp sliyaniya dvoinyh neitronnyh zvezd! Stat'ya opublikovana v Nature (v.426, p.531, 2003). Podrobnee ob etoi rabote mozhno prochitat' v zametke Blinnikova.


Etomu zhe pul'saru posvyashena rabota astro-ph/0312101 (V.Kalogera et al), a obsuzhdeniyu vozmozhnyh scenariev obrazovaniya etoi dvoinoi sistemy - rabota astro-ph/0312152 (J.D.M.Dewi & E.P.J. van den Heuvel).


Vot ona - pervootkryvatel'nica. Marta Burge (v zhizni ona simpatichnee, chem na foto).


astro-ph/0312265 Otdacha pri rozhdenii neitronnyh zvezd iz-za asimmetrii kollapsa (Neutron Star Kicks from Asymmetric Collapse)
Authors: Chris L. Fryer
Comments: 7 pages, 4 figures

Prostranstvennaya skorost' mnogih neitronnyh zvezd prevoshodit 500 km/s. Chtoby ob'yasnit' takie vysokie skorosti predlozheno neskol'ko mehanizmov. Odin iz nih - asimmetriya yadra predsverhnovoi, kotoraya usilivaetsya v hode kollapsa i privodit k asimmetrichnomu vzryvu. V dannoi rabote provodilos' chislenno modelirovanie opisannyh processov. Pravda ochen' vysokih skorostei im poluchit' ne udalos'.

Pozdnyaya stadiya kollapsa yadra sverhnovoi


Vypusk 61. 16-30 noyabrya 2003

astro-ph/0311409 Izmenenie morfologii Krabovidnoi Tumannosti v rentgene na godovyh intervalah vremeni (Year-scale morphological variation of the X-ray Crab Nebula)
Authors: K. Mori et al.
Comments: 6 pages, 2 figures

Kazhdye 1.7 goda Chandra provodit nablyudenii Krabovidnoi tumannosti. Za 3 goda posle zapuska observatorii takih nablyudenii sostoyalos' tri. V tumannosti (v ee detalyah) nablyudayutsya zametnye glazom izmeneniya.


astro-ph/0311415 Pul'sar PSR J1909-3744 - dvoinoi millisekundnyi pul'sar s ochen' malym koefficientom zapolneniya (PSR J1909-3744, a Binary Millisecond Pulsar with a Very Small Duty Cycle)
Authors: B.A.Jacoby et al.
Comments: 12 pages, 4 figures. accepted ApJL

Otkryt odin iz samyh korotkoperiodicheskih millisekundnyh pul'sarov: PSR J1909-3744. Ego osevoi period sostavlyaet vsego 2.95 ms, a orbital'nyi - 1.53 dnya. No samoe interesnoi svoistvo etogo pul'sara - ochen' uzkii impul's, shirina kotorogo sostavlyaet vsego 43 mikrosekundy, chto srazu delaet etot ob'ekt pervym kandidatom v razlichnye vysokotochnye eksperimenty. Na segodnyashnii den' dlya etogo pul'sara uzhe izmereno rasstoyaniya (po parallaksu) d=0.82 kpk i poperechnaya skorost' 140(+80/-40) km/s.


miniobzor astro-ph/0311449 Eshe odno desyatiletie (astro)fiziki strannogo veshestva (Another Decade of Strange Quark Matter (ASTRO) Physics)
Authors: J. E. Horvath, G. Lugones
Comments: 13 pages

Obzor izucheniya kvarkovogo (strannogo) veshestva v 1991-2001 gg. s uporom na astrofiziku (t.e. na strannye zvezdy). Daetsya ochen' horoshee vvedenie v sut' dela. Formul, na udivlenie, ni odnoi. Vsem rekomenduem.


astro-ph/0311498 "Zarubki" na profilyah yarkih pul'sarov ("Notches" in the Profiles of Bright Pulsars)
Authors: M.A.McLaughlin, J.M.Rankin
Comments: 5 pages, 9 figures, submitted to MNRAS. See also astro-ph/0311467.

Na srednih profilyah uzhe treh radiopul'sarov obnaruzheny detali napominayushie "zarubki" (ili "zanozy"). Eto pul'sary J0437-4715, B1929+10 i novyi ob'ekt (kotoromu posvyashena stat'ya) B0950+08. Ranee takie detali ne byli izvestny potomu, chto nablyudeniya s neobhodimoi dlya ih obnaruzheniya tochnost'yu nachaty tol'ko nedavno i detali obnaruzheny u samyh yarkih pul'sarov. (Pri tom, chto nablyudeniya velis' na 300-metrovoi antenne v Aresibo.) Vid etoi detali u pul'sara B0950+08 na chastote 430 MGc pokazan nizhe.


Vypusk 60. 01-15 noyabrya 2003

astro-ph/0311031 Pochemu u millisekundnyh pul'sarov pole slabee, chem u obychnyh? (Why do millisecond pulsars have weaker magnetic fields compared to ordinary pulsars?)
Authors: Arnab Rai Choudhuri, Sushan Konar
Comments: 11 pages, 3 figures

Magnitnye polya millisekundnyh pul'sarov, izmeryaemye po tempu zamedleniya ih vrasheniya, okazyvayutsya sushestvenno nizhe, chem u obychnyh radiopul'sarov. Naibolee rasprostranennoe ob'yasnenie - zatuhanie magnitnogo polya. No est' i drugaya model': napryazhennost' polya v kore neitronnoi zvezdy mozhet byt' toi zhe samoi, no snaruzhi ego pochti ne budet zametno, esli ono "zasypano" sloem akkrecirovavshego na neitronnuyu zvezdu veshestva. Pri vysokoi provodimosti veshestva dostatochno sovsem nebol'shogo ego kolichestva, chtoby na neskol'ko poryadkov oslabit' nablyudaemoe snaruzhi magnitnoe pole. Bolee vazhnym okazyvaetsya vopros o tom budet li ustoichiva situaciya, kogda nad magnitnym polem lezhit sloi veshestva.

Ideya dostatochno staraya i izvestnaya, hotya i ne ochen' populyarnaya. V dannoi rabote provedeno modelirovanie opisannogo effekta ekranirovaniya dlya veshestva s konechnoi provodimost'yu.

Struktura magnitnogo polya "zasypannogo" sloem provodyashego veshestva.


astro-ph/0311121 Pyatnistaya struktura poverhnostnogo magnitnogo polya neitronnoi zvezdy (Spot-like Structures of Neutron Star Surface Magnetic Fields)
Authors: U.Geppert, M.Rheinhardt, J.Gil
Comments: 4 pages, 2 figures

Rentgenovskie i radio nablyudeniya odinochnyh neitronnyh zvezd ukazyvayut na to, chto na poverhnosti etih zvezd mogut sushestvovat' melkomasshtabnye magnitnye polya, na 1-2 poryadka bolee sil'nye, chem dipol'noe magnitnoe pole. Eti polya zametno vliyayut na strukturu akkrecionnyh potokov i oblastei generacii pul'sarnogo izlucheniya, po prakticheski ne skazyvayutsya na processah tormozheniya vrasheniya zvezdy. Avtory ukazyvayut, chto odnoi iz prichin obrazovaniya melkomasshtabnyh polei mozhet byt' effekt Holla. Na risunke privedeno model'noe raspredelenie poverhnostnyh magnitnyh polei.

Eshe odna stat'ya na ochen' blizkuyu temu:
(astro-ph/0311181) V.Urpin, J.Gil
Konvekciya v protoneitronnyh zvezdah i struktura poverhnostnogo magnitnogo polya radiopul'sarov (Convection in protoneutron stars and the structure of surface magnetic fields in pulsars).


astro-ph/0311296 Tyazhelye neitronnye zvezdy? (Heavy Neutron Stars? A Status Report on Arecibo Timing of Four Pulsar-White Dwarf Systems)
Authors: David J. Nice, Eric M. Splaver, Ingrid H. Stairs
Comments: 4 pages, 1 figure.

Opisyvayutsya rezul'taty nablyudenii chetyreh dvoinyh radiopul'sarov v parah s belymi karlikami na radioteleskope v Aresibo. Vazhneishii rezul'tat sostoit v tom, chto dlya odnoi sistemy (PSR J0751+1807) obnaruzhena evolyuciya orbity pod deistviem gravitacionnogo izlucheniya, chto pozvolilo ocenit' massu neitronnoi zvezdy v 1.6-2.8 mass Solnca. Opredelenie mass pul'sarov kraine vazhno dlya opredeleniya "edinstvenno vernogo" uravneniya sostoyaniya neitronnyh zvezd. Eto, v svoyu ochered', ochen' interesno ne tol'ko dlya astronomov, no i dlya fizikov (napomnim, chto plotnost' v nedrah neitronnyh zvezd prevoshodit plotnost' atomnogo yadra v neskol'ko raz!). Esli massa etoi neitronnoi zvezdy i pravda ravna 2.8 mass Solnca (berem verhnii predel), to eto budet potryasayushe interesno i vazhno dlya astrofiziki neitronnyh zvezd i fiziki yadernoi materii.


Vypusk 59. 19-31 oktyabrya 2003

astro-ph/0310483 Zatuhanie magnitnogo polya ili lish' zavisimost' diagrammy napravlennosti ot perioda? (Magnetic field decay, or just period-dependent beaming?)
Authors: Joeri van Leeuwen, Frank Verbunt
Comments: 4 pages, 2 figures. To appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler

Kak izvestno, neitronnye zvezdy - eto svoeobraznye astrofizicheskie laboratorii, gde veshestvo nahoditsya v ekstremal'nom sostoyanii. Poetomu protekanie razlichnyh fizicheskih processov v etih kompaktnyh ob'ektah predstavlyaet obshii interes.

Odnim iz takih processov yavlyaetsya evolyuciya magnitnogo polya. Neitronnye zvezdy obladayut samymi sil'nymi magnitnymi polyami vo Vselennoi (u naibolee zamagnichennyh iz izvestnyh segodnya ob'ektov oni prevoshodyat 1014 Gs). My ne znaem, kak takie polya generiruyutsya (prostym szhatiem s sohraneniem magnitnogo potoka tut ne oboitis'), i ne znaem, kak oni izmenyayutsya so vremenem. Sobstvenno, izmenenie mozhet byt' odno - polya mogut zatuhat'. Polya porozhdayutsya tokami, kotorye tak ili inache dolzhny umen'shat'sya. Vopros v tom naskol'ko bystro i sushestvenno.

Pryamye dannye nablyudenii ne dayut odnoznachnogo otveta o povedenii magnitnogo polya neitronnyh zvezd. Naprimer, molodye pul'sary imeyut neskol'ko bOl'shie polya, chem bolee starye istochniki etogo tipa. No statistika nevelika, a krome togo mogut byt' vazhny raznoobraznye effekty selekcii. Poetomu obychno primenyaetsya modelirovanie - populyacionnyi sintez. I tut tozhe raznye gruppy poluchayut raznye rezul'taty.

Avtory dannoi zametki polemiziruyut s temi, kto govorit o zametnom umen'shenii magnitnogo polya za vremya poryadka 10 millionov let. Kak pokazano v etoi rabote, vvedenie dopolnitel'nogo parametra - zavisimosti shiriny puchka izlucheniya ot perioda vrasheniya neitronnoi zvezdy - pozvolyaet opisat' dannye nablyudenii bez zatuhaniya polya. Takaya zavisimost' imeet pod soboi horoshuyu osnovu, poetomu k rezul'tatam issledovaniya stoit otnestis' ser'ezno.


miniobzor astro-ph/0310509 Budushie vozmozhnosti dlya izucheniya pul'sarov v gamma-diapazone (Future Facilities for Gamma-Ray Pulsar Studies)
Authors: D. J. Thompson
Comments: To appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler

Sovremennaya astronomiya - vsevolnovaya. Lyuboi ob'ekt stremyatsya izuchit' v raznyh diapazonah spektra. Pul'sary - ne isklyuchenie.


Profili impul'sov semi pul'sarov v raznyh diapazonah. Na nizhnei osi ukazan period vrasheniya neitronnoi zvezdy v millisekundah.

V blizhaishie neskol'ko let budet zapusheno neskol'ko kosmicheskih apparatov, kotorye v chastnosti smogut nablyudat' gamma-izluchenie ot odinochnyh neitronnyh zvezd. Ob etom i rasskkazyvaetsya v obzore.


astro-ph/0310665 Otkrytie novogo tranzientnogo kandidata v magnitary: XTE J1810-197 (Discovery of a New Transient Magnetar Candidate: XTE J1810-197)
Authors: A. I. Ibrahim et al.
Comments: Submitted to ApJL; 4 pages; 4 figures

Sobstvenno otkryt novyi rentgenovskii pul'sar s periodom 5.54 sekundy. Period uvelichivaetsya s tempom poryadka 10-11 s/s. Esli eto tormozhenie po magnito-dipol'noi formule, to pole poluchaetsya 3 1014 Gs. Eto magnitarnoe pole. Krome togo, net nikakih sledov vtorogo kompan'ona. Vse vmeste delaet ob'ekt klassicheskim anomal'nym rentgenovskim pul'sarom. Istochnik byl naiden takzhe i v arhivnyh dannyh. No togda on byl gorazdo slabee. Eto oznachaet, chto mozhet byt' dva sostoyaniya anomal'nogo pul'sara: aktivnoe i spokoinoe. A eto, v svoyu ochered', oznachaet, chto mnogo magnitarov mozhet skryvat'sya ot nas.


Vypusk 58. 01-17 oktyabrya 2003

astro-ph/0310142 Magnitovrashatel'nyi mehanizm vzryva sverhnovoi vtorogo tipa (Magnetorotational mechanism of supernova type II exlosion)
Authors: S.G.Moiseenko, G.S.Bisnovatyi-Kogan, N.V.Ardeljan
Comments: 5 pages, 4 figures.

Ocherednaya rabota gruppy uchenyh iz IKI, posledovatel'no izuchayushih magnitovrashatel'nyi mehanizm vzryva sverhnovyh. V etom mehanizme istochnikom energii sluzhit kineticheskaya energiya bystro vrashayusheisya neitronnoi zvezdy, ona peredaetsya sbrasyvaemoi obolochke cherez magnitnoe pole. V postroennoi v rabote modeli energiya vzryva sostavlyaet 1.12x1051 erg, sbrasyvaetsya 0.11 massy Solnca.


astro-ph/0310201 Temp rozhdeniya pul'sarov po Parksovskomu obzoru (Pulsar Birthrate from Parkes Multi-beam Survey)
Authors: N.Vranesevic et al.
Comments:

V obzore, osnovannom na nablyudenii bolee 800 pul'sarov, issledovalsya ne tol'ko obshii temp ih rozhdeniya, no i raspredelenie molodyh pul'sarov po magnitnym polya. Polucheny sleduyushie rezul'taty (dlya noveishei modeli rasstoyanii do pul'sarov Cordes & Lazio (2002)):

Pole
(log B)
 Interval mezhdu rozhd. 
(let)
Chislo v Galaktike

>12.530-7017000
12.0-12.550-11080000
<12.090-250563000

To est' primerno polovina pul'sarov rozhdaetsya s polyami bol'she 3x1012 Gs, no v Galaktike ih nablyudaetsya nemnogo, tak kak oni bystro tormozyatsya i vyklyuchayutsya.


astro-ph/0310224 Akkreciya na bystrye rentgenovskie pul'sary (Accretion Onto Fast X-Ray Pulsars)
Authors: S.A.Rappaport et al.
Comments: 10 pages, 5 figures, submitted to ApJ

V poslednie desyat' let byli otkryty akkreciruyushie rentgenovskie pul'sary s millisekundnymi periodami. V standartnoi modeli akkrecii voznikayut nekotorye problemy s ob'yasneniem nablyudaemyh svoistv etih ob'ektov. Naprimer, s ob'yasneniem togo, chto temp akkrecii u nih razlichaetsya pochti na dva poryadka velichiny, ili chto eti ob'ekty demonstriruyut ochen' vysokie tempy tormozheniya.

Dlya ob'yasneniya nablyudaemyh yavlenii avtory predlagayut modificirovannuyu model' diska u kotorogo vneshnyaya granica raspolozhena na radiuse korotacii. Razmer takogo diska zavisit ot perioda vrasheniya neitronnoi zvezdy.


astro-ph/0310347 Otkrytie dvuh dvoinyh millisekundnyh pul'sarov v sharovom skoplenii M30 (GBT Discovery of Two Binary Millisecond Pulsars in the Globular Cluster M30)
Authors: S.M.Ransom et al.
Comments: 9 pages, 6 figures, submitted to ApJ

V sharovom skoplenii M30 obnaruzheny dva dvoinyh millisekundnyi pul'sara. Eto pervye pul'sary, otkrytye v dannom skoplenii. Pul'sar PSR J2140-2310A (M30A) imeet period 11 ms, orbital'nyi period okolo 4 chasov i krugovuyu orbitu. V etoi sisteme nablyudayutsya zatmeniya pul'sara ionizovannym vetrom vtorogo kompan'ona. Pul'sar PSR J2140-23B (M30B) imeet period 13 ms i skoree vsego vysokoekscentrichnuyu orbitu (ona eshe ne opredelena). Polozhenie etogo pul'sara sovpadaet s rentgenovskim teplovym istochnikom, kotoryi v skoplenii M30 nablyudal Chandra. Nablyudeniya pul'sarov velis' na radioteleskope Green Bank na volne 20 sm.


miniobzor astro-ph/0310451 Nablyudatel'nye proyavleniya molodyh neitronnyh zvezd: pul'sary, pitaemye vrasheniem (Observational manifestations of young neutron stars: Spin-powered pulsars)
Authors: Michael Kramer
Comments: Invited review to appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler, 8 pages, 3 figures
astro-ph/0310454 Novye pul'sary, otkrytye v skanah Aresibo (New Pulsars Discovered in Arecibo Drift-Scan Searches)
Authors: M. A. McLaughlin et al.
Comments: 2 pages, 1 figure. To appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler
astro-ph/0310455 Dva pul'sara s magnitarnymi polyami (Two Radio Pulsars with Magnetar Fields)
Authors: M. A. McLaughlin et al.
Comments: 2 pages. To appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler

Kak obychno posle bol'shoi konferencii poyavlyaetsya mnozhestvo statei, napravlennyh v knigu ee materialov. Tri dovol'no pokazatel'nye raboty. Nachinat' chtenie luchshe s obzora. V nem avtor akkuratno i obstoyatel'no rasskazyvaet o pul'sarah (radio i ne tol'ko) - neitronnyh zvezdah, ch'i nablyudatel'nye proyavleniya svyazany s dissipaciei energii vrasheniya. Zatem v dvuh korotkih zametkah rasskazyvaetsya o novyh otkrytiyah, v tom chisle i o dvuh pul'sarov s ochen' vysokim tempom zamedleniya vrasheniya, chto, kak polagayut, svyazano s bol'shimi magnitnymi polyami.

Vypusk 57. 22-30 sentyabrya

astro-ph/0309523 Rentgenovskoe izluchenie pohozhego na Krab pul'sara PSR J0537-6910 (The X-ray emission of the Crab-like pulsar PSR J0537-6910)
Authors: T. Mineo, G. Cusumano, E. Massaro
Comments: 4 pages, 2 figures

Rentgenovskii pul'sar PSR J0537-6910 ochen' pohozh na pul'sar v krabovidnoi tumannosti, tol'ko ego period sostavlyaet 16 ms (u Kraba - 33 ms). Eto samyi bystryi pul'sar associiruyushiisya s ostatkom sverhnovoi. Krome togo v nem proishodyat chastye i ochen' sil'nye glitchi (skachkoobraznye izmeneniya - "sboi" - perioda vrasheniya). Spektr i profil' rentgenovskogo izlucheniya v diapazone energii 0.1-30 keV vosstanovleny po arhivam BeppoSAX i RossiXTE.


Rentgenovskii profil' impul'sa pul'sara PSR J0537-6910


astro-ph/0309580 Fazy rentgenovskih i radioimpul'sov pul'sara PSR B1937+21 (The phase of the radio and X-ray pulses of PSR B1937+21)
Authors: G. Cusumano et al.
Comments: 5 pages, 2 figures, accepted A&A Lett.

Pul'sar PSR B1937+21 - samyi bystryi izvestnyi millisekundnyi pul'sar s periodom 1.56 ms. On nablyudalsya v rentgene (na BeppoSAX i RXTE) i v radio (na teleskope v Effel'sberge). V oboih diapazonah profil' impul'sa obladaet dvumya pikami. Rentgenovskie impul'sy nemnogo otstayut ot radio, primerno na 50 mikrosekund. Zato s centrami rentgenovskih impul'sov ochen' tochno sovpadayut tak nazyvaemye gigantskie radioimpul'sy vremya ot vremeni voznikayushie na etom pul'sare. Takoe sovpadenie ukazyvaet, chto rentgenovskoe izluchenie i gigantskie radioimpul'sy generiruyutsya v odnoi i toi zhe oblasti magnitosfery pul'sara.

Profili impul'sov pul'sara PSR B1937+21. Vverhu - rentgenovskie dannye RXTE (shirina bina - 16 mikrosekund), v seredine - rentgenovskie dannye BeppoSAX, vnizu - radioimpul'sy. Strelkami pokazany mesta poyavleniya gigantskih radioimpul'sov.


astro-ph/0309588 Vliyanie dvoistvennosti na dinamiku kollapsa yadra i na skorost' neitronnoi zvezdy (The Effects of Binary Evolution on the Dynamics of Core Collapse and Neutron-Star Kicks)
Authors: Ph. Podsiadlowski et al.
Comments: 7 pages, 3 figures, submitted to ApJ

Naibolee mnogochislennye sverhnovye, soglasno zakonu Solpitera, obrazuyutsya iz zvezd s massami okolo 10 Mo. Odnako, ih evolyuciya v odinochnyh i dvoinyh sistemah zametno razlichaetsya. V konce evolyucii v dvoinyh zvezdah s nachal'noi massoi >11 Mo obrazuetsya men'shee zheleznoe yadro, chem v odinochnyh. Zvezdy s massoi 8-11 Mo v dvoinyh sistemah vyzyvayut vzryvy sverhnovyh (kollaps yadra vyzyvaetsya reakciyami elektronnogo zahvata), a odinochnye sistemy takoi massy prevrashayutsya v tyazhelye O-Ne-Mg belye karliki. Estestvennym obrazom voznikayut dve gruppy zvezd: evolyucionirovavshih v tesnyh dvoinyh i odinochnye ili shirokie pary. Vzryvy sverhnovyh pervoi gruppy soprovozhdayutsya men'shei otdachei i, kak sledstvie, porozhdayut neitronnye zvezdy s malymi prostranstvennymi skorostyami.
[Prim.: Konechno, vse eti zaklyucheniya trebuyut dopolnitel'noi proverki.]


astro-ph/0309603 Sistematicheskie variacii momentov prihoda impul'sov ot pul'sara PSR B1937+21 - sledy zvezdy-kompan'ona? (Systematic variation of the residual of PSR B1937+21, the trace of its companion star?)
Authors: B.P.Gong
Comments: 15 pages, 6 tables, 3 figures

PSR B1937+21 - pervyi otkrytyi millisekundnyi pul'sar. Do sih por schitalos', chto on odinochnyi. Odnako dlitel'nye nablyudeniya pokazali, chto momenty prihoda impul'sov ot nego ispytyvali sistematicheskie variacii. Odno iz ob'yasnenii - pul'sar PSR B1937+21 vhodit v dvoinuyu sistemu s kompan'onom massoi okolo 0.01 Mo, orbital'nym periodom poryadka 0.1 dnya, raspolozhennuyu otnositel'no nam "plashmya" s ochen' vysokoi tochnost'yu - vtoroi kompan'on peremeshaetsya po luchu zreniya na 10-4-10-3 svetovoi sekundy (30-300 km). V etom sluchae radial'noe dvizhenie samogo pul'sara pri segodnyashnei tochnosti izmerenii voobshe ne obnaruzhivaetsya. Nablyudaemye otkloneniya momentov prihoda impul'sov svyazany s orbital'noi precessiei neitronnoi zvezdy, os' vrasheniya kotoroi naklonena k ploskosti orbity.


Otkloneniya momentov prihoda impul'sov pul'sara PSR B1937+21
ot ozhidaemyh srednih znachenii za 1984-1993 gg.

[Prim.: Eshe odnim ob'yasneniem nablyudaemyh yavlenii mozhet byt' svobodnaya precessiya pul'sara.]


astro-ph/0309744 Zondirovanie prostranstva-vremeni vokrug Sgr A* s pomosh'yu radiopul'sarov (Probing the Spacetime Around Sgr A* with Radio Pulsars)
Authors: Eric Pfahl, Avi Loeb (CfA)
Comments: 6 pages

Stat'ya primerno na tu zhe temu, chto i predydushaya astro-ph/0309716 (odin iz avtorov - tozhe).

Vokrug central'noi chernoi dyry Mlechnogo Puti (ob'ekta Sgr A*) letayut zvezdy s massami 10-20 Mo. Chem zakanchivaetsya ih evolyuciya? Vzryvami sverhnovyh s obrazovaniem neitronnyh zvezd, kotorye pervye neskol'ko millionov let proyavlyayut sebya kak radiopul'sary. A radiopul'sary - samye tochnye chasy v kosmose!

Ocenki pokazyvayut, chto vokrug Sgr A* dolzhno byt' okolo 1000 radiopul'sarov s periodom obrasheniya men'shim 100 let. Nekotorye iz nih mozhno budet obnaruzhit' na chastotah ~10 GGc, gde maly effekty mezhzvezdnogo rasseyaniya. Esli eto udastsya sdelat', to my ochen' mnogo uznaem o nashei chernoi dyre, vklyuchaya effekty svyazannye s ee vrasheniem.


Vypusk 56. 13-20 sentyabrya 2003

miniobzor astro-ph/0309347 Nablyudatel'nyi obzor akkreciruyushih millisekundnyh rentgenovskih pul'sarov (An observational review of accretion-driven millisecond X-ray pulsars)
Authors: Rudy Wijnands
Comments: 10 pages, 6 figures.

Segodnya izvestno pyat' akkreciruyushih millisekundnyh rentgenovskih pul'sarov. Bol'shuyu chast' obzora zanimaet pul'sar SAX J1808.4-3658 - on byl otkryt pervym i yavlyaetsya samym izuchennym ob'ektom v dannoi gruppe. Ot nego k segodnyashnemu dnyu nablyudalis' uzhe chetyre vspyshki. Poslednyaya iz nih proizoshla v oktyabre 2002 g. i vyzvala osobyi interes, poskol'ku v hode nee u ob'ekta nablyudalis' kilogercovye kvaziperiodicheskie oscillyacii (QPO) odnovremenno na dvuh chastotah i pochti kogerentnye (periodicheskie) pul'sacii vo vremya rentgenovskoi vspyshki pervogo tipa. Do sih por kilogercovye QPO nablyudalis' tol'ko u rentgenovskih novyh - kandidatov v chernye dyry, t.e. v sistemah s kompaktnym ob'ektom ne obladayushim sobstvennym tochno izmerennym periodom vrasheniya. Ostal'nye chetyre ob'ekta etogo klassa byli otkryty v poslednie dva goda, k nastoyashemu vremeni opublikovany rezul'taty tol'ko nebol'shogo kolichestva ih nablyudenii. Vozmozhno, v blizhaishee vremya my poluchim novye interesnye rezul'taty, kasayushiesya etih pul'sarov.

Bolee razvernutuyu i obnovlyaemuyu versiyu dannogo obzora mozhno naiti na saite avtora http://zon.wins.uva.nl/~rudy/admxp/

Ob'ektu SAX J1808.4-3658 takzhe posvyashena stat'ya astro-ph/0309345 "Aperiodicheskoe vremennoe povedenie akkreciruyushego millisekundnogo pul'sara SAX J1808.4-3658"


astro-ph/0309402 Pervye ukazaniya na ciklotronnye detali v spektrah anomal'nyh rentgenovskih pul'sarov (First evidence of a cyclotron feature in an anomalous X-ray pulsar)
Authors: Nanda Rea et al.
Comments: 6 pages, 4 figures.

V avguste 2001 g. rentgenovskii sputnik BeppoSAX provel samye dlitel'nye nepreryvnye nablyudeniya anomal'nogo rentgenovskogo pul'sara 1RXS J1708-4009. V poluchennoi serii spektrov izlucheniya, sinhronnyh s fazoi pul'sacii ob'ekta, na faze, sootvetstvuyushei frontu impul'sa, byla obnaruzhena absorbcionnaya osobennost' (liniya poglosheniya) centr kotoroi prihoditsya na energiyu 8.1 keV. Naibolee veroyatnoe ob'yasnenie podobnoi osobennosti - rezonansnoe ciklotronnoe rasseyanie v magnitnom pole s napryazhennost'yu 9x1011 Gs dlya elektronov ili 1.6x1015 Gs dlya protonov, sootvetstvenno. Esli obnaruzhenie etoi linii budet podtverzhdeno (seichas ee statisticheskaya znachimost' sostavlyaet 4, chto ne ochen' mnogo), to eto budet pervoe obnaruzhenie ciklotronnoi detali u anomal'nyh rentgenovskih pul'sarov (prim. otmetim, pravda, raboty Gavriila i dr. - astro-ph/0209202, astro-ph/0301092 - gde upomyanuta spektral'naya detal' v drugom ARP).

Sprava - faza krivoi bleska na kotoroi byla obnaruzhena spektral'naya osobennost', sleva - usrednennyi spektr s otmechennoi liniei poglosheniya.


astro-ph/0309445 Nablyudeniya pul'sara PSR B1706-44 s XMM-N'yuton (XMM-Newton Observations of PSR B1706-44)
Authors: K.E.McGowan et al.
Comments: 21 pages, 5 figures, 2 tables, accepted for publication in ApJ

Eshe odno ukazanie na sushestvovanie massivnyh neitronnyh zvezd.

Po rezul'tatam nablyudenii 102 ms pul'sara PSR B1706-44 s borta rentgenovskoi observatorii XMM-N'yuton byl postroen spektr ego izlucheniya. Dlya ego approksimacii ispol'zovali kak chernotel'nyi, tak i stepennoi zakony. Eti varianty okazalis' statisticheski nerazlichimymi, no dlya dal'neishego analiza avtory iz fizicheskih soobrazhenii vybrali teplovoi spektr. Esli rasstoyanie do istochnika sostavlyaet ~2.3 kpk, to razmer izluchayushei oblasti dolzhen byt' ravnym ~13 km, chto sravnimo s razmerami neitronnoi zvezdy. Sravnenie poverhnostnoi temperatury takoi zvezdy s krivymi ostyvaniya ukazyvaet na neitronnuyu zvezdu promezhutochnoi, massy ot 1.45 do 1.59 Mo v zavisimosti ot modeli protonnoi sverhprovodimosti ee yadra.

Rezul'tat interesnyi, no ochen' kosvennyi, i vryad li ego mozhno schitat' ser'eznym dokazatel'stvom sushestvovaniya tyazhelyh neironnyh zvezd.


miniobzor nucl-th/0309041 Neitronnye zvezdy dlya studentov (Neutron Stars for Undergraduates)
Authors: Richard R. Silbar and Sanjay Reddy
Comments: 40 pages, 12 figures

Raschet struktury belyh karlikov i neitronnyh zvezd - horoshaya tema dlya studencheskoi kursovoi raboty. Tema zatragivaet razlichnye oblasti fiziki, interesnye kak nachinayushim, tam i bolee opytnym uchenym: ot termodinamiki do kvantovoi statistiki i ot yadernoi fiziki do obshei teorii otnositel'nosti. Resheniya svyazannyh sistem differencial'nyh uravnenii mogut iskat'sya chislenno ili analiticheski, s pomosh'yu paketov simvol'nyh vychislenii, podobnyh "Matematike".

A v samoi stat'e dan kratkii obzor ukazannoi temy, kotoryi mozhet posluzhit' posobiem dlya studenta, vybravshego sebe podobnuyu zadachu.


Vypusk 55. 01-12 sentyabrya 2003

nucl-th/0309022 Effekt cvetnoi sverhprovodimosti na massu i radius kvarkovoi zvezdy (Effect of color superconductivity on the mass and radius of a quark star)
Authors: Stefan B. Ruester, Dirk H. Rischke
Comments: 16 pages, 9 figures

Esli propustit' vtoroi razdel, soderzhashii tehnicheskie detali, to i ne specialistu mozhno uznat' koe-chto interesnoe pro kvarkovye zvezdy. Kratkoe rezyume sostoit iz dvuh punktov. Pervyi v meru banalen: avtory podtverzhdayut rezul'taty drugih issledovanii, chto nalichie cvetnoi sverhprovodimosti (eto kogda kvarki obrazuyut kuperovskie pary, konkretno v ispol'zovavsheisya modeli krasnye i zelenye kvarki obrazuyut anti-sinie kuperovskie pary) ne okazyvaet sushestvennogo vliyaniya na massy i radiusy kompaktnyh ob'ektov pri tipichnyh parametrah. Vtoroi vyvod menee banalen. Avtory zadalis' voprosom, a naskol'ko nado sdvinut' parametry (kotorye mozhno var'irovat' v ramkah sushestvuyushih neopredelennostei), chtoby byl zametnyi effekt. Okazalos', chto mozhno tak sdvinut' parametry, chto radiusy i massy vozrastut vdvoe, no ...... No togda eti kvarkovye zvezdy stanut takimi zhe (po masse i radiusu) kak obychnye neitronnye!

Vypusk 54 23-31 avgusta 2003
miniobzor astro-ph/0308471 Mehanizm izlucheniya pul'sarov (Pulse emission mechanisms)
Authors: Don Melrose
Comments: To appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler

Interesnyi kriticheskii obzor po pul'saram. On v chem-to pereklikaetsya s obzorom Michela, o kotorom my pisali v proshlom vypuske. Osobo vydelim kratkoe opisanie mehanizmov izlucheniya vo vtorom razdele stat'i.


astro-ph/0308455 Mogut li tonkie diski porozhdat' fenomen anomal'nogo rentgenovskogo pul'sara? (Can Thin Disks Produce Anomalous X-Ray Pulsars?)
Authors: K. Yavuz Eksi, M. Ali Alpar Comments: 16 pages, 4 Figures, to be published in Astrophysical Journal Vol. 599, Dec. 10

V poslednie neskol'ko let i s nablyudatel'noi, i s teoreticheskoi tochki zreniya aktivno izuchayutsya odinochnye radiotihie neitronnye zvezdy. Odnoi iz idei, kotoraya po mneniyu ee avtorov mozhet ob'yasnit' srazu neskol'ko klassov nablyudaemyh ob'ektov, yavlyaetsya koncepciya ostatochnogo diska. Posle vzryva sverhnovoi na obrazovavshiisya kompaktnyi ob'ekt mozhet vypadat' bol'shoe (skazhem, 0.1 massy Solnca) kolichestvo vybroshennogo veshestva (t.n. fall-back). Pri etom veshestvo mozhet obrazovavyt' disk vokrug obrazovavsheisya neitronnoi zvezdy. Eto mozhet privodit' kak k razlichnym nablyudatel'nym proyavleniyam, tak i k korrelyacii razlichnyh parametrov neitronnyh zvezd (o poslednem voprose sm. diskussiyu zdes').

Sushestvuet dostatochno mnogo vozrazhenii protiv diskovoi gipotezy v primenenii k anomal'nym rentgenovskim pul'saram i rodstvennym im ob'ektam. V dannoi stat'e avtory pytayutsya otstoyat' svoyu gipotezu. Nekotorye argumenty vyglyadyat dostatochno ubeditel'nymi. Odnako avtory ne obsuzhdayut nekotorye problemy. Naprimer, vopros o vybore parametrov. Model' horosho rabotaet lish' v uzkom diapazone mass akkrecionnogo diska i t.p. Po vsei vidimosti s tochki zreniya razbrosa parametrov teoriya vyglyadit ne ochen' privlekatel'noi, no vremya pokazhet.

Vypusk 53. 10-22 avgusta 2003
astro-ph/0308372 Tri dvoinyh millisekundnyh pul'sara v NGC 6266 (Three Binary Millisecond Pulsars in NGC 6266)
Authors: A.Possenti et al.
Comments: 9 pages, 5 embedded figures, Accepted for publication in ApJ

V sharovom skoplenii NGC 6266 otkryty tri novyh dvoinyh millisekundnyh radiopul'sara. Ih periody ravny 5.2, 3.6 i 3.8 ms, a orbital'nye periody sostavlyayut, sootvetstvenno, 3.8, 0.14 i 0.22 dnya. Orbity vseh treh sistem pochti krugovye (e<10-4). Teper' v etom skoplenii izvestno 6 dvoinyh radiopul'sarov i ni odnogo odinochnogo.


miniobzor astro-ph/0308347 Sovremennoe sostoyanie teorii radiopul'sarov (The State of pulsar theory)
Authors: F. Curtis Michel (Rice Univ., Houston, TX)
Comments: 12 pages, 11 figures, to be published Advances in Space Research

V 10 stranic dannoi stat'i (eshe 2 zanimaet literatura) v ochen' szhatom vide vmestilas' istoriya razvitiya teorii pul'sarov v techenii poslednih 35 let. Polnoi i samosoglasovannoi teorii poka tak i ne udalos' sozdat', no mnogie voprosy poluchili svoe (vozmozhno ne polnoe) reshenie. V ih chislo vhodit ideya o tom, chto plazma dolzhna uskoryat'sya vdol' magnitnyh linii polyarnogo kaspa i drugaya ideya, chto tak nazyvaemyi "pul'sarnyi veter" uskoryaetsya centrobezhnymi silami, a nizkochastotnye elektromagnitnye volny ogromnoi amplitudy ne igrayut v etom processe nikakoi roli. Izobrazheniya pul'sara v Krabe, poluchennye na HST i Chandra ochen' pohozhi na rannyuyu model' Krauze-Polstrofa-Maikela, sostoyashuyu iz dvuh polyarnyh dzhetov i ekvatorial'nogo tora zahvachennoi zaryazhennoi plazmy (t.e. protivorechit raspredeleniyu, vyvedennomu Goldraihom i Dzhulianom, i bol'shinstvu rabot v dannoi oblasti, opublikovannym v poslednie 33 goda).


astro-ph/0308223 Zhestkoe izluchenie ot pul'sarov: trehmernaya geometricheskaya model' (High-Energy Radiation from Pulsars: A Three Dimensional Model Approach)
Authors: K.S. Cheng
Comments: 13 pages, 9 figures

Zhestkoe izluchenie radiopul'sarov porozhdaetsya ul'trarelyativistskimi elektronami dvizhushimisya v iskrivlennom magnitnom pole neitronnoi zvezdy. Elektrony obrazuyutsya v tak nazyvaemom "zazore" - oblasti gde prisutstvuet neskompensirovannoe elektricheskoe pole. V nastoyashee vremya mezhdu soboi konkuriruyut dve gruppy modelei - s vnutrennim i vneshnim zazorami - v pervoi iz nih zazor raspolozhen na poverhnosti pul'sara vblizi ego magnitnyh polyusov, vo vtoroi - vo vneshnih chastyah magnitosfery vblizi svetovogo cilindra.

V modelyah s vneshnim zazorom geometriya magnitosfery (osobenno oblasti kaspa vblizi magnitnyh polyusov) opredelyaet diagrammu napravlennosti zhestkogo izlucheniya i, kak sledstvie, profil' impul'sa radiopul'sara v zhestkom diapazone.

Avtoram dannoi raboty udalos' v ramkah samosoglasovannoi trehmernoi geometricheskoi modeli magnitosfery ob'yasnit' ryad svoistv profilei impul'sov pul'sarov v neskol'kih energeticheskih diapazonah.


Trehmernaya struktura vneshnego zazora, ob'yasnyayushaya nablyudaemye profili izlucheniya pul'sarov v gamma-diapazone


astro-ph/0308148 Neitronnye zvezdy kak sverhprovodniki pervogo tipa (Neutron Stars as Type I Superconductors)
Authors: Kirk B.W. Buckley, Max A. Metlitski, Ariel R. Zhitnitsky
Comments: 5 pages

Neitronnye zvezdy predstavlyayut bol'shoi interes dlya fizikov. V tom chisle dlya teh, kto zanimaetsya fizikoi sploshnyh sred, kondensirovannogo sostoyaniya i t.p. Delo v tom, chto v ih nedrah veshestvo nahoditsya v ochen' interesnyh usloviyah. Tol'ko sudit' o povedenii veshestva prihoditsya po kosvennym priznakam. Naprimer, po svobodnoi precessii radiopul'sarov. Link (Link) schitaet, chto sushestvovanie svobodnoi precessii nesovmestimo s sosushestvovaniem sistemy protonnyh magnitnyh trubok i sistemy neitronnyh vihrei. Rezul'tatom etogo dolzhno sluzhit' razrushenie magnitnyh trubok i vytalkivanie magnitnogo polya iz sverhtekuchego (i sverhprovodyashego) yadra. Takoe povedenie svoistvenno sverhprovodnikam pervogo tipa.

V dannoi stat'e avtory razvivayut etu ideyu. Pokazano, chto pri uchete kuperovskogo sparivniya i protonov, i neitronov, proishodit razrushenie sistemy magnitnyh trubok, chto privodit k tomu, chto vse pole vytalkivaetsya iz yadra. Za schet togo, chto v protonnoi trubke est' pary neitronov, trubki nachinayut ne ottalkivat'sya (kak v sverhprovodnikah vtorogo tipa), a prityagivat'sya.

Sverhprovodimosti v kompaktnyh zvezdah posvyashena takzhe stat'ya "Meissner Effect and Vortex Dynamics in Quark Stars -- A Model for Soft Gamma-Ray Repeaters". V nei avtory predlagayut model' istochnikov myagkih povtoryayushihsya gamma-vspleskov (MPG), osnovannuyu na effekte Meissnera (vytalkivanie magnitnogo polya iz sverhprovodnika) i povedenii vihrei v nedrah kvarkovoi zvezdy. Vytalkivanie magnitnogo polya privodit k peresoedineniyu magnitnyh silovyh linii, t.e. k bystromu vydeleniyu energii.


Vypusk 51. 21-31 iyulya 2003

astro-ph/0307352 Otskok pul'sara iz-za krupnomasshtabnoi anizotropii vzryva sverhnovoi (Pulsar Recoil by Large-Scale Anisotropies in Supernova Explosions)
Authors: L. Scheck et al.
Comments: 4 ps figures, 2 colored, high-quality available upon request

Izvestno, chto neitronnye zvezdy letyat v prostranstve so skorostyami inogda prevoshodyashimi 1000 km/s. Eto mnogo (skorost' zvezd-praroditelei poryadka 30 km/s i ne prevoshodit 100 km/s). Nablyudeniya isklyuchayut vozmozhnost' razgona zvezdy posle vspyshki sverhnovoi. Znachit, imenno pri vzryve kompaktnyi ob'ekt priobretaet svoyu bol'shuyu skorost'. Odin iz naibolee prostyh i deistvennyh mehanizmov - nesimmetrichnyi sbros veshestva - byl predlozhen I. S. Shklovskim bolee 30 let nazad. Est' i drugie idei, svyazannye s magnitnymi polyami, izlucheniem neitrino i t.d.

V svoei rabote avtory predstavlyayut rezul'taty novyh dvumernyh raschetov vzryva sverhnovoi s uchetom razlichnyh gidrodinamicheskih neustoichivostei. Rezul'taty svodyatsya k sleduyushemu. Neustoichivosti sposobny porodit' dostatochnyi uroven' asimmetrii vzryva, chtoby stali vozmozhny skorosti otdachi (kick, recoil) bolee 500 km/s. T.o. mozhno ob'yasnit' vysokie skorosti radiopul'sarov bez privlecheniya dopolnitel'nyh iskusstvennyh predpolozhenii. Otmetim v zaklyuchenie, chto fizika vzryva sverhnovoi ochen' slozhna, a potomu zdes' eshe budut novye rezul'taty.


Vypusk 50. 8-18 iyulya 2003

astro-ph/0307235 Glitchi anomal'nogo rentgenovskogo pul'sara 1RXS J170849.0--400910 (The glitches of the Anomalous X-ray Pulsar 1RXS J170849.0--400910)
Authors: S. Dall'Osso et al.
Comments: submitted to ApJ Main Journal, 27 pages and 6 figures

Izvestno, chto vrashayushiesya neitronnye zvezdy (v pervuyu ochered' obychnye radiopul'sary) demonstriruyut sboi perioda - t.n. glitchi. Sushestvuet neskol'ko mehanizmov, ob'yasnyayushih takie proishestviya. Odin iz naibolee izvestnyh - zvezdotryaseniya. V kore neitronnoi zvezdy nakaplivaetsya mehanicheskoe napryazhenie, zatem kora treskaetsya, chto privodit k izmeneniyu momenta inercii, a sledovatel'no i perioda vrasheniya. Drugaya model' svyazana s vzaimodeistviem kory i sverhtekuchego yadra zvezdy. Dlya ponimaniya togo, kakoi zhe mehanizm imeet mesto v prirode (ili oba imeyut pravo na sushestvovanie), vazhno nablyudat' povedenie perioda posle glitcha - t.n. relaksaciyu.

V dannoi stat'e avtory opisyvayut nablyudenie eshe odnogo sil'nogo glitcha (sila opredelyaetsya po otnositel'nomu izmeneniyu chastoty vrasheniya) u anomal'nogo rentgenovskogo pul'sara. Predydushii sboi byl zaregistrirovan za poltora goda do etogo. Eto dostatochno chasto. Interesnaya osobennost' zaklyuchaetsya v tom, chto processy relaksacii posle dvuh glitchei proishodili sushestvenno po-raznomu. Vozmozhno, dlya ob'yasneniya raznyh sboev perioda dazhe u odnoi neitronnoi zvezdy neobhodimo privlekat' neskol'ko mehanizmov!



Vypusk 49. 01-07 iyulya 2003

astro-ph/0307065 Nablyudeniya neitral'nogo vodoroda vokrug radiotihoi neitronnoi zvezdy RX J0822-4300 v Puppis A (Observations of the neutral hydrogen surrounding the radio quiet neutron star RX J0822-4300 in Puppis A)
Authors: E. M. Reynoso et al.
Comments: 8 pages, 2 ps/eps figures, plus 1 gif figure and 4 jpg figures, MNRAS, in press. Full postscript version with all 7 figures is available at http://www.physics.usyd.edu.au/~simonj/puppis.ps.gz

Po nablyudeniyam na ATCA (Australia Telescope Compact Array) obnaruzhena bipolyarnaya struktura vokrug odinochnoi radiotihoi neitronnoi zvezdy v ostatke sverhnovoi Puppis A. Vozmozhno, chto eto dva dzheta, vybrasyvaemye kompaktnym ob'ektom. Krome togo, avtoram udalos' utochnit' rasstoyanie do ostatka sverhnovoi - 2.2 kpk.


astro-ph/0307023 Pul'sary tipa Chernoi Vdovy: cena nerazborchivosti (Black Widow Pulsars: the Price of Promiscuity)
Authors: A.R. King, M.B. Davies, M.E. Beer
Comments: 6 pages, 2 figures, MNRAS in press

Pul'sar Chernaya vdova - eto tesnaya dvoinaya sistema, sostoyashaya iz neitronnoi zvezdy (millisekundnogo radiopul'sara) i malomassivnogo kompan'ona. Pul'sar isparyaet svoego soseda (sosedku) - otsyuda i nazvanie. Dolya takih sistem gorazdo vyshe sredi zvezd sharovyh skoplenii, chem sredi zvezd polya Galaktiki. Znachit, v skopleniyah deistvuet kakoi-to dopolnitel'nyi mehanizm ih formirovaniya. Skoree vsego - eto zahvat. Prichem ne prosto zahvat. Neitronnaya zvezda, sostavlyayushaya shirokuyu paru s belym karlikom, "menyaet" starogo kompan'ona na novyi. T.o. "gulyayushaya" po skopleniyu zvezda vstupaet "v gravitacionnuyu svyaz'" s opasnoi neitronnoi zvezdoi, a potom .... Otsyuda "cena nerazborchivosti" v zagolovke stat'i.


Vypusk 48. 23-30 iyunya 2003


astro-ph/0306628 Sobstvennoe dvizhenie, vozrast i nachal'nyi period vrasheniya pul'sara PSR J0538+2817 v S147 (Proper motion, age and initial spin period of PSR J0538+2817 in S147)
Authors: M. Kramer et al.
Comments: accepted for publication in ApJ Letters, 13 pages, 3 figures

PSR J0538+2817 - eto obychnyi radiopul'sar s periodom 0.143 sekundy. Novye nablyudeniya pozvolili odnoznachno ustanovit' ego svyaz' s ostatkom sverhnovoi S147, a takzhe izmerit' ego sobstvennoe dvizhenie, chto pozvolyaet opredelit' ego skorost' v kartinnoi ploskosti (kakova skorost' v napravlenii lucha zreniya my ne znaem). Vse eto dovol'no obydenno.... No! Vozrast ostatka izvesten dovol'no horosho - eto 30+/-4 tysyachi let. Vozrasta pul'sarov obychno ocenivayut tak: period delyat na temp zamedleniya vrasheniya. Dlya PSR J0538+2817 eto daet 600 tysyach let. Pri takoi ocenke molchalivo predpolagaetsya, chto nachal'nyi period vrasheniya byl ochen' malen'kim. Yasno, chto v dannom sluchae eto ne tak. Pul'sar rodilsya s periodom, blizkim k nablyudaemomu: - 0.139 sekundy. Vot eto - vazhnaya informaciya. My znaem nachal'nye periody dlya sovsem nebol'shogo kolichestva pul'sarov. I zdes' kazhdoe novoe otkrytie imeet bol'shoe znachenie.

Vypusk 46. 1-15 iyunya 2003

miniobzor nucl-th/0305097 Plotnaya kvarkovaya materiya v kompaktnyh zvezdah (Dense quark matter in compact stars)
Authors: Mark G Alford
Comments: 11 pages, for proceedings of SQM 2003 conference

Kratko izlagayutsya osnovnye ponyatiya, svyazannye s kvarkovymi zvezdami. Vvidu kratkosti izlozheniya i slozhnosti predmeta mnogie veshi trebuyut dopolnitel'nyh poyasnenii, kotorye predlagaetsya iskat' v citiruemyh obzorah. Obzor budet naibolee ponyaten tem, kto ne ponaslyshke znaet o polyah i chasticah, simmetriyah i ih narusheniyah, no eshe pochti nichego ne znaet o kvarkovyh zvezdah. Eti lyudi naidut izlozhenie prozrachnym, posledovatel'nym i t.d. S drugoi storony, obzor ne peregruzhen formulami (ih prakticheski net), poetomu, esli smirit'sya s nepolnym ponimaniem kakih-to terminov (kak to "narushenie kiral'noi simmetrii"), to stat'ya budet dostupna gorazdo bolee shirokomu krugu chitatelei.

astro-ph/0306065 PSR J1847-0130: radiopul'sar s vrashatel'nymi svoistvami magnitara (PSR J1847-0130: A Radio Pulsar with Magnetar Spin Characteristics)
Authors: M. A. McLaughlin et al.
Comments: 6 pages, Accepted by ApJ Letters

Otkryt ochen' interesnyi radiopul'sar. Ego period vrasheniya 6.7 sekundy - eto mnogo. Chtoby takaya neitronnaya zvezda mogla byt' pul'sarom, u nee dolzhno byt' bol'shoe magnitnoe pole. I eto v samom dele tak: 1014 Gs. T.e. po vsem parametram eto magnitar.

Anomal'nye rentgenovskie pul'sary (ARP) i istochniki myagkih povtoryayushihsya gamma-vspleskov (MPG) ne pokazyvayut aktivnosti v radiodiapazone. Teoretiki bystro pridumali, kak v sil'nom pole mozhno podavit' generaciyu radioizlucheniya (v pole, prevyshayushem 4 1013 Gs, vklyuchayutsya razlichnye kvantovye effekty). No nablyudateli otvetili otkrytiem neskol'kih radiopul'sarov, kotorye s tochki zreniya parametrov vrasheniya (period i proizvodnaya perioda) ne otlichayutsya ot ARP i MPG. Vot eshe odin primer. Prichem, primer samyi sil'nyi. U etogo pul'sara samoe sil'noe pole (zametim, chto pole opredelyaetsya po zamedleniyu vrasheniya v ramkah nekotoryh predpolozhenii, no eti predpolozheniya dlya vseh odinakovy, tak chto PSR J1847-0130 "vyigryvaet" po "obshim pravilam").

astro-ph/0306092 Aktivnost' SGR 1900+14 v aprele 2001 g.: svoistva impul'sa i vrasheniya (The 2001 April Burst Activation of SGR 1900+14: Pulse Properties and Torque)
Authors: Woods et al.
Comments: 13 pages, 3 figures, accepted for publication in ApJ
astro-ph/0306091 Aktivnost' SGR 1900+14 v aprele 2001 g.: rentgenovskoe poslesvechenie (The 2001 April Burst Activation of SGR 1900+14: X-ray afterglow emission)
Authors: Feroci et al.
Comments: 18 pages - 2 Figures (one in color) - Astrophysical Journal (Part I), in press

Dve stat'i, posvyashennye vspyshechnoi aktivnosti istochnika myagkih povtoryayushihsya gamma-vspleskov (MPG) SGR 1900+14 v aprele 2001 g. Obsudim v osnovnom pervuyu stat'yu, posvyashennuyu svoistvam impul'sa i vrasheniya.

MPG po vsei vidimosti yavlyayutsya sverhzamagnichennymi neitronnymi zvezdami. SGR 1900+14 - pozhalui samyi izvestnyi iz chetyreh MPG. Etot istochnik byl otkryt v 1979 g. gruppoi Mazeca. V 1998 g. byla zaregistrirovana samaya moshnaya sredi vseh MPG vspyshka. Za neskol'ko minut istochnik vydelil 1044 erg (Solnce vysvechivaet stol'ko za tysyachu let), dostignuv v pike svetimosti 4 1044 erg/s. Vspyshka soprovozhdalas' izmeneniem profilya impul'sa i sushestvennym zamedleniem vrasheniya. V aprele 2001 g. byla zaregistrirovana menee moshnaya vspyshka (1043 erg) dlitel'nost'yu okolo 40 sekund. Posle nee nablyudalos' neskol'ko obychnyh slabyh vspyshek.

Posle vspyshki 2001 g. ne nablyudalos' sushestvennogo izmeneniya profilya impul'sa. Zato posle vspyshki nablyudalos' sushestvennoe zamedlenie perioda vrasheniya. Eto oznachaet, chto velichina zamedleniya ne korreliruet napryamuyu s moshnost'yu (i polnoi energetikoi) vspyshki.

miniobzor astro-ph/0306143 Ostyvanie neitronnyh zvezd: teoreticheskie aspekty i nablyudatel'nye ogranicheniya (Neutron star cooling: Theoretical aspects and observational constraints)
Authors: D. G. Yakovlev et al.
Comments: 10 pages, 3 figures, Proceedings of the 34th COSPAR Scientific Assembly (Adv. Sp. Res., accepted)

Ocherednoi korotkii obzor piterskoi gruppy, posvyashennyi ostyvaniyu neitronnyh zvezd. V stat'yu vklyucheny novye rezul'taty: kak teoreticheskie, tak i nablyudatel'nye. Osobo otmetim udachnoe kratkoe opisanie osnovnyh regulyatorov ohlazhdeniya na raznyh etapah evolyucii.


astro-ph/0306162 Priroda neobychnoi struktury dzheta i diska v Krabovidnoi tumannosti (The origin of peculiar jet-torus structure in the Crab nebula)
Authors: S.S.Komissarov, Y.E.Lyubarsky
Comments: Rejected by Nature, submitted to MNRAS Letters

Kogda rentgenovskie nablyudeniya obnaruzhili v Krabovidnoi tumannosti svetyashuyusya strukturu, sostoyashuyu iz dvuh dzhetov, napravlennyh vdol' osi vrasheniya pul'sara, i diska, prishlos' otkazat'sya ot vseh predydushih MGD teorii, v kotoryh predpolagalas' sfericheskaya simmetriya tumannosti. Teper' kartina predstavlyaetsya sleduyushei: vblizi pul'sara energiya, vydelyayushayasya pri tormozhenii vrasheniya neitronnoi zvezdy, perenositsya elektromagnitnym polem (vektorom Pointinga), chasticy pul'sarnogo vetra nesut tol'ko neznachitel'nuyu chast' etoi energii. Odnako ochen' bystro, eshe do dostizheniya udarnoi volny, kotoraya voznikaet pri stolknovenii relyativistskogo vetra s okruzhayushei mezhzvezdnoi sredoi, sootnoshenie menyaetsya na obratnoe - bOl'shaya chast' energii elektromagnitnogo polya peredaetsya potoku chastic.

Dlya resheniya zadachi o strukture relyativistskogo vetra vokrug pul'sara sushestvuyut horoshie chislennye metody, esli sdelat' nekotorye uproshayushie (no realistichnye) predpolozheniya o strukture magnitnogo polya na bol'shih rasstoyaniyah ot pul'sara. Eto i bylo prodelano avtorami dannoi zametki. Okazalos', chto v ramkah sdelannyh prostyh predpolozhenii udaetsya kachestvenno vosproizvesti nablyudaemuyu v rentgene strukturu tumannosti.

Rentgenovskoe izobrazhenii Krabovidnoi Tumannosti poluchennoi Chandroi Raspredelenie sinhrotronnogo rentgenovskogo Izlucheniya poluchennoi v rabote Komissarova i Lyubarskogo


tol'ko cifry astro-ph/0306232 Razmer i rasstoyanie do neitronnoi zvezdy PSR B0656+14 (The distance and radius of the neutron star PSR B0656+14)
Authors: W.F.Brisken et al.
Comments: 7 pages including 1 figure. Submitted to ApJL. AAStex

S pomosh'yu seti antenn VLA byl izmeren godichnyi parallaks pul'sara PSR B0656+14, kotoryi okazalsya ravnym 3.47+/-0.36 mas, chto sootvetstvuet rasstoyaniyu 288(+33/-27) pk. Znaya etu velichinu mozhno po potoku izlucheniya ot neitronnoi zvezdy opredelit' ee razmer. Esli schitat' izluchenie chernotel'nym, radius okazyvaetsya ravnym R~7-8.5 km. Bolee realistichnye modeli vodorodnyh atmosfer v sil'nom magnitnom pole pozvolyayut uvelichit eto znachenie do ~13-20 km.

Smotri takzhe stat'yu astro-ph/0306235, posvyashennuyu etomu zhe pul'saru.


astro-ph/0306242 Sravnenie izmerennyh parametrov vosstanovleniya posle glitchei v pul'sarah Krab i Vela s predskazaniyami modelei neitronnyh zvezd (A Comparison of Measured Crab and Vela Glitch Healing Parameters with Predictions of Neutron Star Models)
Authors: F.Crawford, M.Demianski
Comments: 8 pages, including 3 figures and 1 table. Accepted in ApJ

Glitchi - eto sboi periodov vrasheniya pul'sarov. Sam sboi proishodit pochti mgnovenno, pri etom period vrasheniya neitronnoi zvezdy skachkom ukorachivaetsya. V techenie nekotorogo vremeni posle sboya (1-3 mesyaca) vrashenie pul'sara tormozitsya bolee bystro, posle chego vosstanavlivaetsya obychnoe znachenie proizvodnoi perioda. Sushestvuyu dve naibolee populyarnye teorii ih vozniknoveniya: teoriya "zvezdotryasenii", svyazyvayushaya sboi s razlomami i perestroikoi kory neitronnoi zvezdy, i teoriya sverhtekuchih neitronnyh zvezd, v kotoroi glitch vyzyvaetsya vyhodom iz sverhtekuchego yadra ocherednogo vihrya (yadro mozhet byt' sverhtekuchim i v pervoi modeli). Eti teorii predskazyvayut raznye znacheniya parametra zatuhaniya glitchei Q. Dlya pervoi modeli velichina Q ravna otnosheniyu momenta inercii sverhtekuchego yadra k polnomu momentu inercii neitronnoi zvezdy. Sovremennaya teoriya stroeniya neitronnyh zvezd govorit, chto dannoe otnoshenie dlya zvezdy standartnoi massy 1.4Mo ne mozhet byt' men'she 0.55.

Bol'shoe chislo sboev vrasheniya nablyudalos' tol'ko u dvuh pul'sarov: v Krabovidnoi tumannosti (PSR B0531+21) i v Parusah (PSR B0833-45). U pervogo iz nih Q lezhit v intervale 0.7-1.0 (za isklyucheniem odnogo glitcha), chto horosho soglasuetsya s teoriei "zvezdotryaseniya". U pul'sara Vela znachenie Q malo (0.03-0.3). Eto podtverzhdaet rezul'taty predydushih issledovanii, utverzhdavshih chto sboi vrasheniya pul'sara Vela vyzyvayutsya drugoi prichinoi.


Vypusk 45. 26-31 maya 2003

astro-ph/0305510 Peremennyi dzhet pul'sara v Parusah (The Variable Jet of the Vela Pulsar)
Authors: G. G. Pavlov, M. A. Teter, O. Kargaltsev, D. Sanwal
Comments: 13 pages, including 10 figures and 2 tables, accepted for publication in ApJ. The Vela Pulsar Jet movie and full resolution images are avaliable at http://www.astro.psu.edu/users/pavlov/vela_jet_movie.html

Mozhno nichego ne pisat' - posmotrite mul'tfil'm.

Pul'sar v Parusah (Vela) eto molodaya neitronnaya zvezda - vozrast okolo 10000 let. Kak i u Kraba, u Vely vidyat dzhet. Prichem dzhet vedet sebya, kak hvostik u igrivogo shenka, kak govorit molodezh' - kolbasit.

Blagodarya novoi tehnike (Chandra, Habbl i vse-vse-vse) stalo vozmozhnym ochen' detal'noe izuchenie pul'sarnyh tumannostei. I zdes' uchenyh zhdalo neskol'ko syurprizov, naprimer tor u Kraba i vot "vihlyayushii" dzhet u Vely.

Prosmatrivaya mul'tfil'm obratite vnimanie na letyashie sgustki... (inache, kak pisal Koz'ma, vse eto budet pustym zanyatiem).

O poiskah tumannosti v opiticheskom diapazone sm. otdel'nuyu stat'yu "Search for the Optical Counterpart of the Vela Pulsar X-ray Nebula" (kratkii vyvod: tumannost' v optike ne obnaruzhena).

Vypusk 44. 17-23 maya 2003

astro-ph/0305306 Istoriya dvuh sliyanii: poiski strannosti v kompaktnyh zvezdah (A Tale of Two Mergers: Searching for Strangeness in Compact Stars)
Authors: Madappa Prakash and James M. Lattimer
Comments: 10 pages with 6 figures

Plotnost' v centre neitronnoi zvezdy primerno na poryadok velichiny prevyshaet yadernuyu (takoe povyshenie plotnosti vyzvano sobstvennoi gravitaciei neitronnoi zvezdy) Segodnya my vse eshe ne znaem svoistv yadernoi materii nastol'ko horosho, chtoby skazat', chto imenno mozhet proishodit' v centrah neitronnyh zvezd. Etot fakt sluzhit odnoi iz prichin togo, chto v astrofizike uzhe neskol'ko let konkuriruyut drug s drugom modeli neitronnyh zvezd i strannyh zvezd (sm., naprimer, zdes'). Okazalos', odnako, chto razlichit' ih nablyudatel'no dostatochno tyazhelo. Avtory dannoi stat'i predlagayut svoi podhod, oni rassmotreli dve tesnye slivayushiesya sistemy, v kazhduyu iz nih vhodit chernaya dyra massoi M=3.5Mo, no v odnoi ih nih vtorym komponentom yavlyaetsya "obychnaya" neitronnaya zvezda, a v druguyu strannaya kvarkovaya zvezda (obe massoi M=1.5Mo).

Evolyuciya etih sistem do zapolneniya zvezdami svoih polostei Rosha idet absolyutno odinakovo, zatem nachinaetsya peretekanie veshestva na chernuyu dyru. (Avtory polagayut, chto peretekanie idet stacionarnym obrazom, chto dostatochno razumno pri vysokom otnoshenii mass v etih sistemah.) Dal'neishaya evolyuciya sistem dostatochno sil'no razlichaetsya - strannaya zvezda bystree priblizhaetsya i slivaetsya s chernoi dyroi. Na grafike pokazany zavisimosti mass zvezd (M), ih radiusov (R) i poluosei sistem (a) ot vremeni (sploshnye linii - strannaya zvezda, punktir - neitronnaya).

Mozhet byt' detektory gravitacionnyh voln smogut nakonec naiti strannye zvezdy?


Vypusk 43. 12-16 maya 2003

astro-ph/0305273 Pul'sar Vela v blizkom IK (The Vela Pulsar in the Near-Infrared)
Authors: Y.A.Shibanov, A.B.Koptsevich, J.Sollerman, P.Lundqvist
Comments: 12 pages, 8 figures

Vela (Parusa) - samyi izvestnyi pul'sar posle Kraba. V blizkom IK ego udalos' pronablyudat' vpervye (v fil'trah H i Js). Nablyudeniya velis' na odnom iz 8.2-m teleskopov VLT v Chili.

V vydutoi pul'sarnym vetrom tumannosti udalos' obnaruzhit' dva slabyh ob'ekta na rasstoyanii okolo 1.5" na yugo-zapad i severo-vostok ot pul'sara, t.e. po i protiv napravleniya ego dvizheniya. Pohozhe, chto eto dzhety pul'sara (tochnee dzhet i kontrdzhet), ranee obnaruzhennye v rentgene. Oba ob'ekta ochen' krasnye i v optichesom diapazone ne vidny.

Eshe odnim otkrytiem stal tot fakt, chto spektr v blizkom IK lozhitsya na prodolzhenie zhestkogo "hvosta" izlucheniya pul'sara i sovershenno ne pohozh na chernotel'nuyu sostavlyayushuyu, prevaliruyushuyu v optike i myagkom rentgene.

astro-ph/0305256 Teplovaya struktura i ohlazhdenie sverhtekuchih zamagnichennyh neitronnyh zvezd (Thermal structure and cooling of superfluid magnetic neutron stars)
Authors: A.Y.Potekhin, D.G.Yakovlev, G.Chabrier, O.Y.Gnedin
Comments: 15 pages, 12 figures, 2 tables; accepted for publication in ApJ

Gruppa astrofizikov iz Fiziko-Tehnicheskogo instituta im. A.F.Ioffe (Sankt-Peterburg) pochti dvadcat' let sistematicheski i ochen' uspeshno zanimaetsya izucheniem neitronnyh zvezd - v pervuyu ochered' voprosami ih ostyvaniya. Dannaya rabota ne soderzhit nichego "osobenno novogo", prosto ispol'zovany ispravlennye znacheniya razlichnyh parametrov (neprozrachnostei, teploprovodnostei i t.d.) i sobrana voedino pochti vsya fizika, kotoraya rabotaet vnutri ili na poverhnosti ostyvayushih neitronnyh zvezd: izluchenie neitrino, teploprovodnost' neitronnogo veshestva, perehod protonov v yadre i/ili neitronov v kore v sverhtekuchee sostoyanie, uchet vliyaniya akkrecii na atmosferu i koru neitronnoi zvezdy, vliyanie sverhsil'nyh (vyshe kvantovogo predela) magnitnyh polei, uchet dipol'noi struktury magnitnogo polya, kak vnutri neitronnoi zvezdy, tak i na poverhnosti i mnogoe drugoe. V etoi rabote osoboe vnimanie udeleno malomassivnym zvezdam, v kotoryh ne vklyuchayutsya pryamye urka-processy i kotorye iz-za etogo dolgo ostayutsya goryachimi. Sil'noe vliyanie na ih ohlazhdenie okazyvayut namagnichivanie obolochki iz naakkrecirovannogo veshestva i neitronnaya sverhtekuchest' v kore zvezd. Novye rezul'taty vazhny dlya pravil'noi interpretacii nablyudenii naibolee goryachih (dlya svoego vozrasta) odinochnyh neitronnyh zvezd, takih kak RX J0822-43 ili PSR B1055-52.

astro-ph/0305235 Gigantskii impul's ot pul'sara PSR B0540-69 v Bol'shom Magellanovom Oblake (Giant Pulses from PSR B0540-69 in the Large Magellanic Cloud)
Authors: Simon Johnston, Roger W. Romani
Comments: Accepted by ApJ Letters. 11 pages, 3 figures

My uzhe pisali i o gigantskih impul'sah i o poiskah takovyh ot vnegalakticheskih ob'ektov. I vot - pervyi uspeh. Obnaruzhen gigantskii pul's ot pul'sara v Magellanovom oblake. Energiya impul'sa v 5000 raz bol'she srednei energii ipmul'sa ot etogo istochnika.

miniobzor astro-ph/0305249 Strannaya kvarkovaya materiya v neitronnyh zvezdah - novye rezul'taty s Chandry i XMM (Strange Quark Matter in Neutron Stars? - New Results from Chandra and XMM)
Authors: Markus H. Thoma, Joachim Truemper, Vadim Burwitz
Comments: 7 pages, 4 figures, to be published in the SQM 2003 proceedings

Desyat' let nazad kvarkovye zvezdy kazalis' redkostnoi ekzotikoi. Teper' vse izmenilos'. Est' dovol'no mnogo horoshih kandidatov, i dannye so sputnikov Chandra i N'yuton prodolzhayut podkidyvat' drova v plamya diskussii o real'nosti etih strannyh strannyh ob'ektov.

Sobstvenno, stat'ya posvyashena tomu, chto v svete novyh dannyh stalo namnogo legche i estestvennee interpretirovat' nekotorye ob'ekty kak obychnye neitronnye zvezdy, nesoderzhashie sushestvennogo kolichestva kvarkovoi materii.


astro-ph/0305157 Opticheskoe otozhdestvlenie SAX J1808.4-3658 v spokoinom sostoyanii: ukazaniya na aktivnyi radiopul'sar? (The Optical Counterpart to SAX J1808.4-3658 in Quiescence: Evidence of an Active Radio Pulsar?)
Authors: L.Burderi et al.
Comments: 4 pages, A&A Letters, in press

V 2001 g. Gomerom i dr. (Homer et al.) dvoinoi millisekundnyi rentgenovskii SAX J1808.4-3658 byl otozhdestvlen so zvezdoi velichinoi V=21.5. Nablyudeniya velis' v spokoinom sostoyanii istochnika (u kotorogo sluchayutsya dostatochno moshnye vspyshki). Ob'ekt pokazal sinusoidal'nuyu modulyaciyu s 6% amplitudoi i periodom ravnym orbital'nomu periodu pul'sara. Obychnaya model' podobnoi sistemy vyglyadit tak: osnovnoi vklad v postoyannuyu opticheskuyu svetimost' daet izluchenie akkrecionnogo diska vokrug kompaktnogo ob'ekta, a peremennost' vyzvana "effektom otrazheniya" - tem, chto storona normal'noi zvezdy, povernutaya k pul'saru, bolee goryachaya iz-za oblucheniya (irradiacii) zhestkim izlucheniem. Odnako dlya dannoi sistemy eto ob'yasnenie ne podhodit, tak kak takaya amplituda effekta otrazheniya trebuet v 10-50 raz bol'shego potoka zhestkogo izlucheniya, chem nablyudaetsya ot dannoi sistemy v ee spokoinom sostoyanii. Poetomu avtorami byla predlozhena drugaya model', soglasno kotoroi neitronnaya zvezda v dannoi sisteme perehodit v sostoyanie ezhekcii (ispuskaet potoki relyativistskih chastic za schet tormozheniya osevogo vrasheniya) v spokoinom sostoyanii. Progrev vtorichnogo kompan'ona osushestvlyaetsya imenno etim potokom chastic i parametry dannoi modeli udaetsya polnost'yu soglasovat' s nablyudeniyami. Nizkaya amplituda opticheskoi peremennosti yavlyaetsya pervym ukazaniem na prisutstvie v dannoi sisteme aktivnogo radiopul'sara.


Vypusk 41. 25-30 aprelya 2003


astro-ph/0304487 Spektral'nye svoistva anomal'nyh rentgenovskih pul'sarov (Spectral properties of anomalous X-ray pulsars)
Authors: Y. Lu, W. Wang, Y. Zhao
Comments: 10 pages, 3 figures, 1table, submitted to Chin. J. Astron. Astrophys.

Hotya seichas osnovnoi gipotezoi, ob'yasnyayushei svoistva anomal'nyh rentgenovskih pul'sarov (ARP) i istochnikov povtoryayushihsya gamma-vspleskov (MPG), yavlyaetsya sverhzamagnichennaya neitronnaya zvezda - magnitar, tem ne menee akkrecionnaya gipoteza ne zakryta okonchatel'no. T.e. mozhno pytat'sya interpretirovat' svoistva etih kraine interesnyh ob'ektov, ispol'zuya akkreciyu veshestva na neitronnye zvezdy.

V dannoi rabote avtory obsuzhdayut korrelyaciyu mezhdu tempom zamedleniya ARP i ih spektral'nymi svoistvami. Poluchennye rezul'taty pozvolyayut opisat' etu zavisimost' i dlya ARP, i dlya MPG v ramkah akkrecionnoi modeli. Otmetim, odnako, chto vse-taki akkrecionnaya gipoteza vstrechaet ryad trudnostei, i navernoe korrelyaciyu zamedlenie-spektr udastsya opisat' i v ramkah scenariya so sverhzamagnichennymi neitronnymi zvezdami.


Vypusk 40. 20-25 aprelya 2003

miniobzor astro-ph/0304372 Izmenenie povedeniya istochnikov myagkih povtoryayushihsya gamma-vspleskov (The Dynamic Behavior of Soft Gamma Repeaters)
Authors: Peter M. Woods (USRA/NSSTC)
Comments:Invited review to appear in "High Energy Studies of Supernova Remnants and Neutron Stars" (COSPAR 2002). 12 pages, 7 figures

Istochniki myagkih povtoryayushihsya gamma-vspleskov (MPG) - eto, po vsei vidimosti, sil'no zamagnichennye molodye neitronnye zvezdy s periodami vrasheniya poryadka 5-10 sekund. V spokoinom sostoyanii oni nablyudayutsya kak slabye rentgenovskie istochniki (i vo mnogom pohozhi na anomal'nye rentgenovskie pul'sary). No inogda oni ispytyvayut gigantskie vspyshki. Sobstvenno i otkrytie etogo klassa ob'ektov svyazano s takoi vspyshkoi 5 marta 1979 g., zaregistrirovannoi apparaturoi na sputnike serii Venera i na drugih sputnikah. V nastoyashee vremya izvestno chetyre takih istochnika.

V nebol'shom obzore privedeno mnogo interesnyh dannyh po izmeneniyam svoistv MPG posle vspyshek. Eto variacii profilei impul'sov, izmenenie potoka, izmenenie perioda vrasheniya.


astro-ph/0304365 Poisk gigantskih impul'sov ot vnegalakticheskih radiopul'sarov (Searches for Giant Pulses from Extragalactic Pulsars)
Authors: J. M. Cordes, M. A. McLaughlin
Comments: 12 pages, Submitted to ApJ

My uzhe pisali o gigantskih impul'sah radiopul'sarov. V etoi stat'e (svyazannoi s predydushei) avtory obsuzhdayut vozmozhnost' obnaruzheniya takih vspleskov ot vnegalakticheskih pul'sarov. Oni opisyvayut provedennye poiski (v napravlenii na M33, Bol'shoe Magellanovo oblako i pyat' drugih galaktik) gigantskih impul'sov. Rezul'tat poka otricatel'nyi - vspleski ne obnaruzheny - no otmetim, chto eto pervaya ser'eznaya popytka v etom napravlenii. Sootvetstvenno avtory opisyvayut metodologiyu poiska i voznikayushie trudnosti.


Vypusk 39. 12-18 aprelya 2003


astro-ph/0304233 Registraciya v infrakrasnom diapazone anomal'nogo rentgenovskogo pul'sara 1RXS J1708-4009 (The IR counterpart to the Anomalouos X-ray Pulsar 1RXS J1708-4009)
Authors: G.L.Israel et al.
Comments: ApJ Letters, in press, 5 pages and 3 figures

Avtory soobshayut o tom, chto im udalos' otozhdestvit' anomal'nyi rentgenovskii pul'sar (ARP) 1RXS J1708-4009 v infrakrasnom diapazone na Kanadsko-Francuzskom Gavaiskom teleskope. Velichina ob'ekta ravna K'=17.53 (v polose K'). Peremennost' ne obnaruzhena. Potok izlucheniya v IK vyshe, chem predskazyvalo prodolzhenie teplovogo spektra iz rentgenovskoi oblasti. Veroyatno, eto obshee svoistvo ARP, tak kak u vseh chetyreh otozhdestvlennyh v IK ob'ektov nablyudaetsya izbytok izlucheniya v etom diapazone.

astro-ph/0304205 Bol'shoi vsplesk, podobnyi MPG, i sboi perioda u Bol'she-Ne-Stol'-Anomal'nogo Rentgenovskogo Pul'sara 1E 2259+586 (A Major SGR-like Outburst and Rotation Glitch in the No-Longer-So-Anomalous X-ray Pulsar 1E 2259+586)
Authors: V. M. Kaspi et al.
Comments: Accepted for publication in ApJ Letters. 12 pages, 2 figures

Poyavlyayutsya vse novye i novye argumenty v pol'zu togo, chto Anomal'nye rentgenovskie pul'sary (ARP) i istochniki myagkih povtoryashihsya gamma-vspleskov (MPG) - bliznecy-brat'ya. T.o. nakaplivayutsya argumenty v pol'zu "edinyh modelei", v pervuyu ochered' v pol'zu magnitarnoi. Takie scenarii opisyvayut ARP i MPG kak rodstvennye ob'ekty, ili nahodyashiesya na raznyh evolyucionnyh statdiya, ili imeyushie nemnogo raznye parametry. Magnitary - sil'nozamagnichennye neitronnye zvezdy. Teoriya takih ob'ektov seichas aktivno razvivaetsya. Poka eto nailuchshaya gipoteza, opisyvayushaya ARP i MPG.

Nablyudeniya na sputnike RXTE pokazali nalichie u ARP 1E 2259+586 vspyshek, vo mnogom podobnyh vspyshkam MPG. Krome togo, neitronnaya zvezda ispytala sboi perioda - glitch. Chastota vrasheniya rezko uvelichilas' (izmenenie perioda pri glitche ne ochen' bol'shoe, no esli vy predstavite sebe volchok s massoi Solnca, plotnost'yu atomnogo yadra, razmerom v 10 km i periodom v neskol'ko sekund, to stanet yasno, chto dazhe nebol'shoe izmenenie perioda trebuet mnogo usilii). Takzhe uvelichilsya i temp zamedleniya vrasheniya, kotoryi vernulsya k prezhnemu urovnyu lish' spustya 18 dnei. Odnovremenno byli provedeny opticheskie i IK nablyudeniya. Tam takzhe bylo otmecheno uvelichenie potoka. Eta osobennost' poka ne opisyvaetsya v magnitarnoi modeli Tompsona i dr. Otsutstvie zhe gamma-vspyshki pri nalichii rentgenovskoi mozhno ob'yasnit' igraya svoistvami magnitnogo polya (mul'tipol'nost'yu) i svoistvami kory.



Vypusk 38. 01-11 aprelya 2003

astro-ph/0304088 Shirokaya absorbcionnaya detal' v rentgenovskom spektre odinochnoi neitronnoi zvezdy RBS1223 (1RXS J130848.6+212708) (A broad absorption feature in the X-ray spectrum of the isolated neutron star RBS1223 (1RXS J130848.6+212708))
Authors: F. Haberl et al.
Commets: 6 pages, LaTex, accepted A&A Letters

Kak my uzhe mnogo raz pisali, HMM-N'yuton obladaet potryasayushimi spektral'nymi vozmozhnostyami. Vot eshe odno tomu podtverzhdenie.

Nablyudeniya odinochnoi neitronnoi zvezdy RBS1223 (odnoi iz "velikolepnoi semerki") pokazali nalichie interesnoi spektral'noi detali. Delo v tom, chto hotya vsem ochevidno, chto velikolepnaya semerka- eto sem' odinochnyh neitronnyh zvezd, ih priroda ostaetsya vo mnogom neyasnoi. Slishkom malo informacii. Naprimer, my ne znaem, kakie u nih magnitnye polya. Dannaya zhe detal' v spektre mozhet byt' interpretirovana kak protonnaya ciklotronnaya liniya, sootvetstvuyushaya polyu (2-6) 1013 Gs. Krome togo, detal'nye spektry mogut pomoch' luchshe ponyat' svoistva atmosfery etoi neitronnoi zvezdy, chto kritichno dlya ponimaniya ee prirody.

miniobzor! astro-ph/0304120 Fizicheskie processy v sil'nyh magnitnyh polyah neitronnyh zvezd (Physical Processes in Strong Magnetic Fields of Neutron Stars)
Authors: Alice K. Harding
Commets: 11 pages, invited talk at Pulsars, AXPs and SGRs Observed with BeppoSAX and Other Observatories, Marsala, Sicily, Sept. 2002

Ochen' horoshii i ponyatnyi obzor, vklyuchayushii v sebya kratkoe opisaniya vseh vazhnyh processov, proishodyashih v sil'nyh magnitnyh polyah neitronnyh zvezd.

Istoriya izucheniya neitronnyh zvezd so sverhsil'nymi magnitnymi polyami nachinaetsya s 1992 g., kogda byli opublikovany raboty Usova i Dunkana, Tompsona. Poslednie i predlozhili termin "magnitar".

V polyah vyshe 4.4 1013 Gs stanovyatsya vozmozhnymi mnogie ekzoticheskie processy (naprimer, raspad fotona na dva - t.n. photon spliting). I eto nablyudaetsya! My znaem neitronnye zvezdy s polyami do 1015 Gs.

Dlya teh, kto hochet bol'she uznat' o vsei etoi interesnoi fizike, kak raz podhodit dannyi korotkii obzor.


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