The R.A.P. Project (Reviews of Astro-Ph)
Neitronnye zvezdy
Authors: M. S. Jackson et al.
Comments: 22 pages including 7 figures
Neitronnye zvezdy byvayut samymi raznymi: eto i radiopul'sary; i anomal'nye rentgenovskie pul'sary; i radiotihie neitronnye zvezdy i t.d. i t.p. (sm. obzor na russkom yazyke v astro-ph/0205298).
Sredi vsego etogo zooparka osoboe mesto zanimaet Geminga. Po vsei vidimosti eto molodaya odinochnaya neitronnaya zvezda, yavlyayushayasya radiopul'sarom, no radio luch ne prohodit cherez zemnogo nablyudatelya (isklyucheniem yavlyaetsya nizkochastotnaya oblast', gde Geminga byla zaregistrirovana Pushinskimi astronomami).
V dannoi stat'e avtory privodyat rezul'taty glubokih nablyudenii Gemingi v zhestkom diapazone na sputnikah ASCA , RXTE i CGRO.
V rabote obsuzhdaetsya povedenie neitronnoi zvezdy posle glitcha, t.e.
sboya perioda vrasheniya. Rezul'taty interpretiruyutsya v modeli vneshnego zazora
(outer-gap). Obsuzhdayutsya dal'neishie nablyudeniya.
Authors: Umin Lee, Shijun Yoshida
Comments: 20 pages, 12 figures. To appear in ApJ
Neskol'ko let nazad, v 1998 g., bol'shoe vnimanie specialistov privlekli t.n. r-mody neustoichivosti, voznikayushei v molodyh vrashayushihsya neitronnyh zvezdah. Pri etom izluchayutsya gravitacionnye volny i, sootvetstvenno, zamedlyaetsya vrashenie neitronnoi zvezdy. Takaya neustoichivost' mogla by byt' opredelyayushei pri formirovanii raspredeleniya nachal'nyh periodov vrasheniya neitronnyh zvezd.
Odnako, usloviya vozniknoveniya neustoichivosti, intensivnost' izlucheniya i t.p. voprosy v prilozhenii k real'nym neitronnym zvezdam ostayutsya neizvestnymi v svyazi s tem, chto neizvestny s bol'shoi tochnost'yu parametry veshestva v neitronnyh zvezdah. V dannoi stat'e avtory issleduyut problemu v sluchae nalichiya sverhtekuchekogo yadra. Pokazano, chto mogut sozdavat'sya usloviya, kogda r-mody stanovyatsya neustoichivymi.
Authors: G.L. Comer
Comments: 53 pages, LaTeX using REVTeX4. To appear in a special issue of Foundations of Physics in honor of Jacob Bekenstein
Kak mozhno zaglyanut' vnutr' neitronnoi zvezdy, tuda gde veshestvo po vsei vidimosti nahoditsya v sverhtekuchem sostoyanii? Takuyu vozmozhnost' v principe dayut issledovaniya raznoobraznyh kolebanii neitronnyh zvezd. Avtor obsuzhdaet, chto mozhno uznat' o vnutrennem stroenii neitronnyh zvezd pri registracii gravitacionnyh voln, ispuskaemyh pri glitchah i drugih (v pervuyu ochered' neradial'nyh) kolebaniyah neitronnyh zvezd.
Authors: Eric M. Splaver et al.
Comments: Accepted by ApJ, 10 pages, 5 figures
Horoshii primer togo, kak opredelyayut massy neitronnyh zvezd. Naibolee tochno eto udaetsya sdelat' v dvoinyh sistemah, gde odin iz kompan'onov - radiopul'sar (vtoraya, chashe vsego, belyi karlik).
V rassmatrivaemoi sisteme po nablyudeniyu effektov OTO udaetsya opredelit' summu mass. Ona okazalas' ravnoi 2.81 +/- 0.30 mass Solnca. Zatem, s uchetom drugih effektov, a takzhe predpolozheniya o prirode vtoroi zvezdy, udaetsya dat' ocenki mass komponent. Massa neitronnoi zvezdy ocenena kak 1.70(+0.59 -0.63) massy Solnca, a massa belogo karlika - 0.97(+0.43 -0.24). Zamechu, chto v predelah oshibok massa neitronnoi zvezdy sovmestima s "klassicheskim" znacheniem 1.4 massy Solnca.
Razumeetsya, udalos' ocenit' i drugie parametry sistemy i ee komponent, no eto uzhe ne stol' interesno ...
Authors: R. Hollerbach, G. R\"{u}diger
Comments: 10 pages, 12 figures, Mon. Not. R. Astron. Soc., accepted
V astrofizike neitronnyh zvezd mnogo nereshennyh voprosov. Odin iz nih - zatuhanie magnitnogo polya. Molodye neitronnye zvezdy imeyut bol'shie polya, starye (millisekundnye pul'sary) - malen'kie. Znachit, vozmozhno pole zatuhaet. Odnako, po nablyudeniyam radiopul'sarov nel'zya sdelat' odnoznachnogo vyvoda o nalichii ili otsutstvii zatuhaniya. Eto otkryvaet prostor dlya teoretikov.
T.k. my dazhe ne znaem gde sosredotocheno pole (v yadre ili v kore neitronnoi zvezdy), to modelei mozhet byt' mnozhestvo. V svoei stat'e avtory rassmatrivayut pole v kore, zatuhayushee za schet omicheskih poter' (eto standartnaya kartina) plyus deistvuet hollovskii dreif. Vyvody stat'i neodnoznachny. Veroyatno, chto hollovskii dreif vse-taki uskoryaet raspad polya.
Authors: J.L. Zdunik
Comments: accepted for publication in A&A
V stat'e poluchena ocenka minimal'nogo radiusa strannoi zvezdy s koroi iz obychnogo veshestva. V zavisimosti ot razlichnyh predpolozhenii rezul'tat okazyvaetsya poryadka 4-5 km. On sootvetstvuet masse <0.1 massy Solnca.
Authors: B. Willems, U. Kolb
Comments: Accepted by MNRAS, 15 pages, a version with higher resolution figures can be downloaded from http://phys-ftp.open.ac.uk/pub/publications/S20020445282596/bmsp.ps.gz
Millisekundnye pul'sary mogut obrazovyvat'sya razlichnymi sposobami. V svoei rabote avtory rassmatrivayut chetyre puti obrazovaniya millisekundnyh pul'sarov v shirokih (period bolee 1 dnya) dvoinyh sistemah. Dlya sravneniya model'nyh populyacii s dannymi nablyudenii avtory ispol'zuyut raspredeleniya po orbital'nym periodam. Pri nekotoryh predpolozheniyah avtoram udaetsya dostich' horoshego soglasiya raschetov i nablyudenii. Odnako, kak oni sami ukazyvayut, ostaetsya problema s ob'yasneniem dvoinyh s periodami menee 20 dnei.
Authors: W.Becker , G.G.Pavlov
Comments: 45 pages, 19 figures, Review on high energy observations of isolated Neutron Stars. To appear in "The Century of Space Science", eds. J.Bleeker, J.Geiss, M.Huber, Kluwer Academic Publishers, in press.; Original from January 2001, revised refereed version from December 2001. The paper with high resolution images can be obtained from ftp://ftp.xray.mpe.mpg.de/people/web/Becker_Pavlov.pdf
Zamechatel'nyi obzor po nablyudeniyam odinochnyh neitronnyh zvezd (kak radiopul'sarov, tak i radiotihih) v zhestkom diapazone. Dannye po rentgenovskim nablyudeniyam sushestvenno bolee polnye, chem v nashem obzore (isklyuchaya radiotihie neitronnye zvezdy). Ochen' rekomenduyu.
Authors: Alice K. Harding
Comments: 10 pages, invited paper at XXXVIIth Rencontres de Moriond "The Gamma-Ray Universe", March 9-16, 2002, Les Arcs, France
My znaem o neitronnyh zvezdah ochen' mnogo - my znaem o neitronnyh zvezdah ochen' malo. V nastoyashii moment bOl'shaya chast' nablyudaemyh neitronnyh zvezd - radiopul'sary. Odnako, etim vse ne ischerpyvaetsya. Est' samye raznye tipy neitronnyh zvezd. I daleko ne vse iz nih horosho izucheny. Est' nebol'shaya gruppa ob'ektov (7+4 kandidata): neitronnye zvezdy nablyudayushiesya v gamma-diapazone. O nih i rasskazyvaetsya v obsuzhdaemom obzore.
Vse sem' istochnikov i chetyre kandidata, obsuzhdaemye v stat'e, yavlyayutsya bolee-menee obychnymi radiopul'sarami. Avtor rassmatrivaet razlichnye mehanizmy izlucheniya, kotorye mogut byt' otvetstvennymi za gamma-izluchenie neitronnyh zvezd. Krome togo rassmatrivayutsya radiotihie neitronnye zvezdy, a takzhe neotozhdestvlennye gamma-istochniki.
Ozhidaetsya, chto novye sputniki (GLAST i dr.) smogut uvidet' v gamma-diapazone neskol'ko desyatkov radiopul'sarov.
Authors: W. Becker, B. Aschenbach
Comments: 23 pages, 22 figures, 4 tables. To appear in the Proceedings of the 270.WE-Heraeus Seminar on Neutron Stars, Pulsars and Supernova Remnants, Jan 21-25, Physikzentrum Bad Honnef, eds W. Becker, H. Lesch & J. Truemper. Proceedings available as MPE-Report 278. The paper with high resolution images can be obtained from ftp://ftp.xray.mpe.mpg.de/people/web/Becker_Aschenbach.pdf
Dan obzor nablyudenii neitronnyh zvezd i pul'sarov na sputnike HMM-N'yuton.
Authors: F. Pacini
Comments: 3 pages. To appear in the Proceedings of the 270. WE-Heraeus Seminar on Neutron Stars, Pulsars and Supernova Remnants, Jan. 21-25, 2002, Physikzentrum Bad Honnef, eds W. Becker, H. Lesch & J. Truemper. Proceedings are available as MPE-Report 278
Odnovremenno poyavilos' mnozhestvo materialov seminara po neitronnym zvezdam, pul'saram i ostatkam sverhnovyh. Statei ochen' mnogo, poetomu ukazhem lish' nekotorye. Obzor po nablyudeniyam radiopul'sarov daetsya v zametke Vilebinskogo. Mehanizmy izlucheniya radiopul'sarov obsuzhdayutsya Lyubarskim. Interesnyi istochnik, Geminga-2, opisan v stat'e Reimera i dr. Drugie stat'i legko naiti, zadav v pole "Comments" slovosochetanie "WE-Heraeus".
Authors: D.G. Yakovlev, P. Haensel
Comments: 5 pages, 2 figures
astro-ph/0209027 Thermal state of transiently accreting neutron stars
Authors: D.G. Yakovlev, K.P. Levenfish, P. Haensel
Comments: 7 pages, 2 figures
Dve stat'i ot piterskoi gruppy issledovatelei neitronnyh zvezd. Gruppa izvestna v pervuyu ochered' svoimi raschetami ohlazhdeniya neitronnyh zvezd. Imenno etoi probleme i posvyasheny obe stat'i.
V pervoi stat'e obsuzhdayutsya odinochnye neitronnye zvezdy s razlichnym veshestvom v ih yadrah. Vo vtoroi rassmatrivayutsya zvezdy v dvoinyh sistemah, gde proishodyat epizody akkrecii, mezhdu kotorymi mozhno nablyudat' poverhnost' ostyvayushego kompaktnogo ob'ekta.
Authors: I. Vida\~na, I. Bombaci, A. Polls, A. Ramos
Comments: Submitted to Astronomy & Astrophysics
Issleduyutsya ochen' molodye neitronnye zvezdy (t.n. protoneitronnye zvezdy). V ramkah vybrannogo podhoda avtory v chastnosti pokazyvayut, chto takie ob'ekty s gravitacionnoi massoi ot 1.28 do 1.59 mass Solnca yavlyayutsya metastabil'nymi i pozzhe kollapsiruyut, prevrashayas' v malomassivnye chernye dyry.
Authors: Madappa Prakash et al.
Comments: pages, 1 figure, uses espcrc1.sty (included)
Izvestie o tom, chto istochniki RX J185635-3754 i 3C58 mogut byt' kvarkovymi zvezdami dolgo budorazhilo sredstva massovoi informacii (sm. sootvetstvuyushie raz'yasneniya na Astronete i Scietific.Ru).
V korotkoi zametke izvestnye specialisty po vnutrennemu stroeniyu neitronnyh zvezd obsuzhdayut vozmozhnosti nablyudatel'nyh proyavlenii (i, sootvetstvenno, ih registracii) kvarkovyh zvezd.
Authors: F. P. Gavriil, V. M. Kaspi, P. M. Woods
Comments: 14 pages, 2 figures, accepted for publication in Nature. Note: The content of this paper is embargoed until 1900 hrs London time / 1400 US Eastern Time on Sept 11
Opisyvaetsya otkrytie dvuh rentgenovskih vspyshek ot anomal'nogo rentgenovskogo pul'sara 1E 1048-5937. Vspyshki ochen' pohozhi na vspyshki istochnikov povtoryayushihsya gamma-vspleskov. Eto delaet eshe bolee veroyatnoi tesnuyu svyaz' mezhdu anomal'nymi rentgenovskimi pul'sarami i istochnikami povtoryayushihsya gamma-vspleskov.
Authors: Feryal Ozel, Dimitrios Psaltis
Comments: 8 pages, submitted to The Astrophysical Journal Letters
Na profili spektral'nyh linii, izluchaemye neitronnymi zvezdami, vliyaet mnozhestvo effektov teorii otnositel'nosti. Sootvetstvenno, poluchiv izmereniya linii, mozhno srazu zhe uznat', naprimer, massu i radius neitronnoi zvezdy. K sozhaleniyu, poka takie linii uvidet' ne udalos'. Delo za nablyudatelyami.
Authors: S. V. Bogovalov, D.V. Khangoulian
Comments: 7 pages, 1 figure. accepted to MNRAS
Avtory rassmatrivayut obrazovanie tora i dzhetov vokrug pul'sara v Krabe. Novoe, chto vvodyat avtory, - anizotropiya potoka energii ot pul'sara.
Authors: M.E.Gusakov, O.Y.Gnedin
Comments: 10 pages, 6 figures
Journal-ref: Astronomy Letters 28 (2002) 669-675
Authors: Yasufumi Kojima, Koh-ichi Sakata
Comments: 8 pages, 4 figures, accepted for publication in Prog. Theor. Phys
Kak otlichit' obychnuyu neitronnuyu zvezdu ot kvarkovoi? Idei mnogo. Vot eshe odna. U kvarkovyh i neitronnyh zvezd okazyvayutsya razlichnymi kolebatel'nye svoistva. Esli udast'sya (v otdalennom budushem!) pronablyudat' gravitacionnye volny ot oscilliruyushih kompaktnyh ob'ektov, to mozhno budet otlichit' kvarkovye zvezdy ot neitronnyh (otmechu, odnako ot sebya, chto volny proshe nablyudat' ot tol'ko chto sformirovavshihsya zvezd, a perehod v kvarkovoe sostoyanie mozhet proizoiti namnogo pozzhe).
Authors: D. K. Kaplan, S. R. Kulkarni, M. H. van Kerkwijk
Comments: 4 pages, 2 figures. Uses emulateapj5.sty, onecolfloat5.sty. Accepted by ApJ Letters
Vsego dva ob'ekta iz "velikolepnoi semerki" radiotihih blizkih neitronnyh zvezd obnaruzheny v optike. Glubokie poiski na Kosmicheskom teleskope, vozmozhno, dali eshe odnogo opticheskogo dvoinika. Eto stalo vozmozhnym blagodarya nablyudeniyam istochnika na Chandre (u Chandry ochen' malen'kii boks oshibok). Kak i u drugih istochnikov opticheskii spektr lezhit vyshe chernotel'nogo prodolzheniya rentgenovskogo spektra. Eto mozhet ob'yasnyat'sya atmosferoi neitronnoi zvezdy.
Comments: 7 pages, 3 figures. Uses emulateapj5.sty, onecolfloat5.sty. Submitted to ApJ
Anomal'nye rentgenovskie pul'sary (ARP) i istochniki myagkih povtoryayushihsya gamma-vspleskom (MPG) - bliznecy-brat'ya. Polagayut, chto oba tipa ob'ektov - magnetary. Nablyudeniya SGR 0526-66 na Chandre v spokoinom sostoyanii podtverzhdayut "rodstvo". Klassicheskii MPG vedet sebya seichas kak obychnyi ARP.
Authors: Frank Verbunt
Comments: 10 pages, three figures, to appear in New Horizons in Globular Cluster Astronomy, Eds. Piotto et al., ASP Conf. Ser
Sharovye skopleniya stali odnoi iz osnovnyh mishenei sputnikov Chandra i N'yuton. Eto privelo k sushestvennomu uvelicheniyu kolichestva izvestnyh rentgenovskih istochnikov. Frank Verbunt, odin iz vedushih issledovatelei v etoi oblasti, daet nebol'shoi, no ischerpyvayushii obzor obrazovaniya i evolyucii tesnyh dvoinyh sistem s neitronnymi zvezdami v sharovyh skopleniyah. Takzhe kratko obsuzhdayutsya sistemy s belymi karlikami i chernymi dyrami.
Authors: T. Di Salvo, L. Burderi
Comments: 6 pages, submitted to A&A
Polucheny ogranicheniya na velichinu magnitnogo polya dlya dvuh neitronnyh zvezd, vhodyashih v tesnye dvoinye sistemy. Dlya SAX J1808.4-3658 obnaruzheny pul'sacii na chastote 400 Gc. Eti dannye pozvolyayut utverzhdat', chto pole zaklyucheno v uzkom intervale ot 108 do 5 108Gs. Dlya vtoroi sistemy, Aql X-1, polucheno, chto pole ne prevoshodit 109Gs.
Authors: Nicholas D. Lyford, Thomas W. Baumgarte, Stuart L. Shapiro
Comments: 6 pages, to appear in ApJ
Neitronnye zvezdy (osobenno molodye) obladayut differencial'nym vrasheniem. Eto privodit k uvelicheniyu maksimal'noi vozmozhnoi massy. Dannaya situaciya i issleduetsya avtorami. V chastnosti vazhnym okazyvaetsya sluchai slivayushihsya neitronnyh zvezd, kotorye bez effektov diff.vrasheniya dolzhny bystro kollapsirovat' v chernuyu dyru.
Authors: D.R. Lorimer (JBO), F. Camilo (Columbia), P. Freire (NAIC), M. Kramer (JBO), A.G. Lyne (JBO), R.N. Manchester (ATNF) and N.D'Amico (Cagliari Observatory)
Commets: 4 pages, 1 figure, to appear in proceedings of the conference "Radio Pulsars" held in Chania, Crete, Sept 2002
Segodnya v sharovom skoplenii 47 Tukana izvestny 22 millisekundnyh radiopul'sara.
V stat'e priveden kratkii obzor ih svoistv. Opisana istoriya nablyudenii skopleniya.
Periody: vse pul'sary imeyut periody ot 2 do 8 ms. Otsutstvie pul'sarov s bOl'shimi
periodami - real'nyi effekt. Pul'sarov s periodami 1-2 ms tozhe malo i eto
ne effekt selekcii.
Dvoinye pul'sary: 68% (15 iz 22) pul'sarov vhodyat v
dvoinye sistemy. Bol'shinstvo sistem otnositsya k odnoi iz dvuh grupp -
s orbital'nym periodom 0.4-2.3d i kompan'onami s massoi ~0.4Mo
i s orbital'nymi periodami 1.5-5.5h i menee massivnym kompan'onom
(~0.2Mo).
Astrometriya: Horosho izvestny polozheniya 15 pul'sarov. Vse oni
raspolozheny ne dalee, chem v 1.2" ot centra skopleniya (eto 4 radiusa ego yadra).
Takaya koncentraciya govorit, chto pul'sary dostigli teplovogo ravnovesiya
otnositel'no dvizhenii v skoplenii.
Tablic net, no dany ssylki na original'nye raboty.
Authors: Alaa I. Ibrahim, Samar Safi-Harb, Jean H. Swank, William Parke, Silvia Zane, Roberto Turolla
Commets: Published in the 2002 July 20 issue of the Astrophysical Journal Letters, 574, L51 Journal-ref: Published in the 2002 July 20 issue of the Astrophysical Journal Letters, 574, L51
S borta RXTE v spektre SGR 1806-20 byla zaregistrirovana ciklotronnaya osobennost'. Detal' sostoit iz iz uzkoi linii poglosheniya na energii 5 keV i nekotoroi modulyacii spektra vblizi 2-i i 3-i garmonik (11.2 keV i 17.5 keV). Ekvivalentnaya shirina linii okolo 500 eV. Liniya byla vidna tol'ko v samoi zhestkoi chasti prekursora vspyshki. Takaya liniya sootvetstvuet magnitnomu polyu na poverhnosti B=(5-7)x10{11}Gs, chto sovershenno ne pohozhe (ochen' malO) dlya SGR. Odnako, esli eto protonnaya ciklotronnaya liniya, to pole budet ravno B=1.0x10{15}Gs, chto horosho ob'yasnyaet nablyudaemyi period etogo ob'ekta. source.
Authors: Peter D. Edmonds (CfA)
Commets: 8 pages, 2 figures. To appear in New Horizons in Globular Cluster Astronomy, eds. G. Piotto, G. Meylan, G. Djorgovski, & M. Riello, ASP Conference Series
Nablyudeniya sharovyh skoplenii s Habblovskogo kosmicheskogo teleskopa i s rentgenovskogo sputnika Chandra privelo k tomu, chto v otdel'nyh skopleniyah bylo otkryto bolee 10, a v otdel'nyh sluchayah i bolee 100, rentgenovskih dvoinyh istochnikov s neitronnymi zvezdami. V etom obzore osnovnoe vnimanie udeleno obnaruzheniyu etih istochnikov, ih opticheskoi identifikacii, poisku millisekundnyh pul'sarov i malomassivnyh rentgenovskih dvoinyh v spokoinom sostoyanii.
Authors: Valeria Ferrari, Giovanni Miniutti, Jose' A. Pons
Comments: submitted to MNRAS, 24 pages
Novorozhdennye neitronnye zvezdy (vozrast menee minuty) sushestvenno otlichayutsya ot bolee "zrelyh" ob'ektov etogo tipa. Eto goryachie, neprozrachnye dlya neitrino shary. Za neskol'ko sekund oni izluchayut kolossal'nuyu energiyu. Bol'shaya chast' unositsya neitrino, no nekotoraya dolya unositsya gravitacionnymi volnami.
V etoi stat'e avtory rassmatrivayut process izlucheniya gravvoln molodymi neitronnymi zvezdami. Pokazano, chto esli neitronnaya zvezda rozhdaetsya v nashei Galaktike, to ee gravizluchenie mozhet byt' zaregistrirovano uzhe pervym pokoleniem lazernyh interferometrov. Krome togo, obrazuyushiesya v rezul'tate sliyaniya dvuh neitronnyh zvezd bolee massivnye, t.n. "supramassivnye", neitronnye zvezdy mogut yavlyat'sya bolee moshnymi istochnikami gravitacionnogo izlucheniya. Oni mogut byt' zaregistrirovany na rasstoyaniyah, sootvetstvuyushih skopleniyu v Deve, chto daet temp poryadka neskol'kih shtuk v god.
Authors: David J. Nice, Eric M. Splaver (Princeton), Ingrid H. Stairs (UBC)
Commets: 6 pages, to appear in proceedings of "Radio Pulsars," Chania, Crete, August 2002 (ASP conference series)
Pul'sar - ochen' tochnye "chasy" - na orbite v dvoinoi sisteme pozvolyaet srazu opredelit' funkciyu mass vtorogo komponenta (t.e. poluchit' ogranicheniya na nee snizu). Dlya togo, chtoby izmerit' massu samogo pul'sara neobhodimo zaregistrirovat' odni iz relyativistskih effektov:
- Relyativistskuyu precessiyu orbity. Dlya etogo ee ekscentrisitet dolzhen byt' dostatochno velik.
- Zaderzhka Shapiro - zapazdyvanie impul'sa, kogda luch prohodit ryadom so vtorym telom. Trebuetsya, chtoby orbita byla vidna pochti s rebra.
- Umen'shenie poluosi orbity iz-za izlucheniya gravitacionnyh voln. Effekt zameten tol'ko u samyh tesnyh sistem.
Authors: R. Oechslin, G. Poghosyan, K. Uryu
Commets: 3 Pages, 4 Figures, Proc. Nuclei in the Cosmos 7, 2002
Ochen' kratko opisyvaetsya problema nalichiya kvarkovogo veshestva v slivayushihsya neitronnyh zvezdah. T.k. gravitaconnyi signal mozhet dat' nekotoruyu informaciyu o vnutrennem stroenii neitronnyh zvezd, to predstavlyaet interesnyh rassmotret' stol' modnuyu seichas gipotezu o strannoi materii.
Authors: I.N. Mishustin, M. Hanauske, A. Bhattacharyya, L.M. Satarov, H. Stoecker and W. Greiner
Commets: Latex, 14 pages including five postscript figures
My ne znaem kak vedet sebya veshestvo pri plotnostyah poryadka 1015 g/sm3, kotorye dostigayutsya v centrah neitronnyh zvezd. Teorii predlagayut neskol'ko variantov. Odin iz nih - chto pri dostizhenii opredelennoi plotnosti proishodit dekonfainment kvarkov i v zvezde obrazuetsya yadro iz svobodnyh kvarkov (tochnee iz kvark-glyuonnoi plazmy). A chto pri etom proizoidet s neitronnoi zvezdoi?
Avtory rassmatrivali dostatochno prostuyu dvuhkomponentnuyu model' i var'irovali parametr uravneniya sostoyaniya, otvechayushii za energiyu dekonfainmenta. Bylo obnaruzheno, chto zvezdy s kvarkovymi yadrami imeyut men'shie radiusy i maksimal'nye massy, chem chisto neitronnye zvezdy (podobnye rezul'taty byli izvestny i ran'she). Neozhidannym yavlyaetsya rezul'tat, chto v opredelennom uzkom intervale znachenii parametra uravneniya sostoyaniya udalos' postroit' 2 ustoichivye posledovatel'nosti zvezd s kvarkovymi yadrami, otlichayushiesya drug ot druga razmerami yadra. Mezhdu zvezdami etih posledovatel'nostei vozmozhen bystryi perehod, kotoryi budet soprovozhdat'sya vydeleniem primerno 1052 erg energii. Perehod budet soprovozhdat'sya vspyshkoi neitrinnogo izlucheniya i neskol'ko zaderzhannoi po vremeni vspyshkoi gamma-luchei.
Authors: I. H. Stairs et al.
Comments: 4 pages; to appear in proceedings of "Radio Pulsars," eds. M. Bailes, D. J. Nice, S. E. Thorsett
Kak mozhno tochno dokazat', chto vy otkryli imenno chernuyu dyru? Akkreciruyushie sistemy ne dayut takoi odnoznachnosti (hotya my, na samom dele, i uvereny v sushestvovanii chernyh dyr v tesnyh dvoinyh i v yadrah galaktik). Gravitacionnye detektory (LIGO, VIRGO) eshe ne zarabotali. Mikrolinzirovanie? Vozmozhno, no tut vy ne mozhete otozhdestvit' ob'ekt posle nablyudenii. Vladimir Mihailovich Lipunov uzhe davno propogandiroval ideyu o tom, chto luchshii sposob - eto naiti dvoinuyu sistemu radiopul'sar + chernaya dyra. Po raschetam s pomosh'yu "Mashiny Scenariev" poluchalos', chto takie sistemy dolzhny vstrechat'sya v kolichestve odna shtuka na 1000 radiopul'sarov. Ne tak uzh i malo! My znaem seichas bol'she 1000 pul'sarov. No otkrytie takoi dvoinoi - delo sluchaya. Odnako, ideya pronikla v massy, i potomu radioastronomy ne zabyvayut o tom, chto u nih est' shans poluchit' nobelevskuyu premiyu (navernyaka, za otkrytie takoi sistemy, tochnee za dokazatel'stvo sushestvovaniya chernyh dyr, premiyu mogut dat'). Potomu, otkrytyi v 1997 g. pul'sar 1740-3052 privlekal vnimanie. Delo v tom, chto u nego yavno est' massivnyi kompan'on, no nablyudayushayasya v napravlenii etogo pul'sara zvezdochka po svoim svoistvam emu " ne para". Potomu v svoei stat'e 2001 g. Sterz i dr. predpolozhili, chto vtorym kompan'onom mozhet byt' chernaya dyra. Drugaya vozmozhnost', kotoraya takzhe byla ukazana avtorami - eto massivnaya V-zvezda (kstati, takie pary uzhe obnaruzhivalis', i ih tozhe zapodozrivali v "chernodyrnosti"). V obsuzhdaemoi zametke avtory vse-taki pokazyvayut, chto eto i v samom dele V-zvezda, a ne chernaya dyra. Avtory obnaruzhili sushestvennoe uvelichenie mery dispersii, chto estestvennym obrazom ob'yasnyaetsya vetrom ot massivnoi V-zvezdy. Zhal', znachit otkrytiya radiopul'sara v pare s chernoi dyroi nado eshe zhdat'.... No avtoram dolzhno byt' eshe bolee pechal'no - oni-to mogli rasschityvat' na Nobelevskuyu premiyu :)
Authors: D. R. Lewis et al.
Comments: 4 pages, 2 figures, to appear in proceedings of "Radio Pulsars," Chania, Crete, August 2002 (ASP conference series)
V Avstralii, na gore Udovol'stviya (Mt. Pleasant) s pomosh'yu 26-metrovoi antenny provoditsya regulyarnyi monitoring 10 molodyh radiopul'sarov s cel'yu obnaruzheniya sboev perioda (glitchei). Esli udast'sya obnaruzhit' takoi sboi, to srazu zhe nachnutsya nablyudeniya posleglitchevogo progreva v drugih diapazonah (v pervuyu ochered' - v rentgenovskom).
Krome togo, uzhe 21 god idut nablyudeniya pul'sara Vela na 14-metrovoi antenne (18 chasov v den'!), a takzhe pul'sara PSR B1641-45. Vela daet sboi primerno kazhdye 1000 dnei. U etogo istochnika obnaruzheno uzhe nemalo glitchei. Takie nablyudeniya neobhodimy potomu, chto sboi perioda i ego posleduyushee vosstanovlenie - eto unikal'naya vozmozhnost' uznat' chto-nibud' o "vnutrennostyah" neitronnyh zvezd.
Authors: N. Andersson
Commets: invited review article for Class Quantum Grav., 47 pages, 16 ps figures
V obzore rech' idet o neustoichivostyah v neitronnyh zvezdah (v pervuyu ochererd' v molodyh), privodyashih k izlucheniyu gravitacionnyh voln. V principe takie volny (esli povezet) mozhno zaregistrirovat' s pomosh'yu stroyashihsya interferometrov.
Authors: Roger W. Romani
Commets: 7 pages, 3 figures, to appear in proceedings of the conference "Radio Pulsars" held in Chania, Crete, Sept 2002
V zametke rech' v pervuyu ochered' idet ne o teplovom, a o magnitosfernom izluchenii molodyh pul'sarov. Eto pul'siruyushee, t.e. napravlennoe izluchenie - sushestvuet puchok. Avtor pytaetsya skonstruirovat' nekuyu "edinuyu" model' (podobno opisaniyu aktivnyh yader galaktik), gde v zavisimosti ot orientacii osei pul'sara otnositel'no lucha zreniya poluchalis' by raznye spektry i krivye bleska.
Authors: D.G. Yakovlev, K.P. Levenfish
Comments: 12 pages, 1 figure, uses sc3conf.sty, to appear in Proc. Third Sakharov Conference on Physics, A.Semikhatov et al. (eds.), Scientific World, Moscow (2003)
V otlichii ot termoyadernogo goreniya (nevysokaya plotnost', vysokie temperatury) piknoyadernoe gorenie proishodit pri vysokoi plotnosti i otnositel'no nizkih temperaturah (t.e. v ramkah dannoi zadachi temperaturu mozhno polozhit' ravnoi 0, no eto ne znachit, chto my imeem delo s absolyutnym nulem, napomnim, chto v nekotoryh zadachah vnutrennie chasti neitronnyh zvezd mozhno schitat' nahodyashimisya pri nulevoi temperature, naprimer, yadro neitronnoi zvezdy mozhet byt' sverhtekuchim, no real'naya temperatura tam. po zemnym merkam, ochen' vysokaya). Takie usloviya realizuyutsya, naprimer, v kore akkreciruyushei neitronnoi zvezdy. Veshestvo opuskaetsya v oblast' bolee vysokoi plotnosti pod davleniem svezhevypavshego veshestva.
Rezhim piknoyadernogo goreniya mozhet byt' vazhen dlya zvezd, akkreciya na kotorye nepostoyanna. Togda vo vremya nulevoi akkrecii zvezda budet prodolzhat' svetit' za schet piknoyadernyh reakcii. Seichas eto vpolne nablyudaemaya vesh'.
Authors: J. Cottam et al.
Comments: Published in Nature (Nov 7, 2002)
My ne znaem tochnoe uravnenie sostoyaniya veshestva v neitronnyh zvezdah. Zdes' osobenno zametno skazyvaetsya "nelaboratornost'" astronomicheskih ob'ektov. Dlya neitronnyh zvezd my ne imeem ni odnogo tochnogo odnovremennogo izmereniya massy i radiusa (est' tochnye izmereniya mass, no v etih sluchayah radius neizvesten). Horoshii sposob poluchit' takie dannye - nablyudenie krasnogo gravitacionnogo smesheniya spektral'nyh linii. I ne zrya takoi rezul'tat popal v Nature. Konechno, pryamo iz dannyh po krasnomu smesheniyu nel'zya odnovremenno izvlech' radius i massu. No drugie dannye v itoge pomogayut eto sdelat'.
Avtory nablyudali istochnik EXO 0748-676. Eto tesnaya dvoinaya s akkreciruyushei neitronnoi zvezdoi. Periodicheski proishodyat rentgenovskie vspyshki. Udalos' uvidet' neskol'ko smeshennyh linii v rentgenovskom spektre. z=0.35.
Rezul'tat sootvetstvuet noramal'noi neitronnoi zvezde (nikakoi kvarkovoi ekzotiiki i t.p.).
Authors: S.M.Ransom, J.W.T.Hessels, I.H.Stairs et al.
Commets: 4 pages. To appear in "Radio Pulsars" (ASP Conf. Ser.), eds M. Bailes, D. Nice, & S. Thorsett
S pomosh'yu 300-m radioteleskopa Aresibo i obnovlennogo teleskopa Grin Benk na volne 20 sm byli issledovany 19 sharovyh skoplenii. V nih byli otkryty eshe 7 novyh millisekundnyh radiopul'sarov. 2 iz niz odinochnye, 5 - vhodyat v tesnye dvoinye sistemy. Tri dvoinye sistemy iz pyati obladayut ekscentrichnymi orbitami, a odna iz nih skoree vsego soderzhit relyativistskii kompan'on (belyi karlik ili neitronnuyu zvezdu). Rabota prodolzhaetsya.
Authors: Bennett Link
Comments: 7 pages, to appear in proceedings of "Radio Pulsars", Chania, Crete, August 2002 (ASP conference series)
Odinochnym neitronnym zvezdam mozhet byt' prisusha precessiya. Svyazano eto s napryazheniyami v kore i yadre neitronnoi zvezdy, kotorye privodyat k nesferichnosti zvezdy (prichem, razumeetsya, ob'ekt dolzhen vrashat'sya ne vokrug svoei glavnoi osi). Seichas est' dva kandidata (radiopul'sary), u kotoryh vozmozhno vidyat etot effekt.
Nablyudeniya precessii mogut dat' vazhnuyu informaciyu o fizike neitronnyh zvezd. Naprimer, mozhno opredelit' zavisimost' mezhdu tempom zamedleniya pul'sara i uglom mezhdu magnitnoi os'yu i os'yu vrasheniya. Esli precessiruet bystrovrashayushayasya neitronnaya zvezda, to my mozhem rasschityvat' na registraciyu gravitacionnyh voln.
V stat'e (kotoraya po suti predstavlyaet soboi miniobzor) daetsya vvedenie, poyasnyayushee chto takoe svobodnaya precessiya, a takzhe kak vyglyadit precessiya pri deistvii zamedlyayushei sily. I, konechno zhe, obsuzhdayutsya precessiruyushie neitronnye zvezdy.
Authors: J. Carriere, C.J. Horowitz, J. Piekarewicz
Commets: 9 pages and 5 eps. figures (included)
Teoriya govorit nam, chto holodnye neitronnye zvezdy mogut imet' massy ot 0.1 massy solnca do 2-3 solnechnyh mass. Nablyudeniya svidetel'stvuyut o tom, chto mozhet sushestvovat' rezkii pik na masse 1.35 mass solnca. Malomassivnuyu neitronnuyu zvezdu ochen' trudno sdelat', t.k. dlya ochen' goryachego ob'ekta minimal'naya massa okazyvaetsya vyshe. I potomu obychnye sposoby obrazovaniya neitronnyh zvezd vryad li dayut ob'ekty s massoi men'she solnechnoi. A zhal'! T.k. eto bylo by po svoemu ochen' interesno. Po-krainei mere tak schitayut avtory stat'i. Delo v tom, chto plotnost' v nedrah obychnyh neitronnyh zvezd prevoshodit yadernuyu v neskol'ko raz. Znachit, izmeriv massu i radius takoi neitronnoi zvezdy, my poluchim vazhnuyu informaciyu o povedenii veshestva pri takih plotnostyah (uravnenie sostoyaniya). No kak byt' s men'shei plotnost'yu? Neitronnye zvezdy tut (poka?) ne pomogut. Zdes', pishut avtory, na pomosh' prihodyat laboratornye izmereniya. Izmereniya radiusa neitrona v yadre svinca dayut informaciyu o povedenii veshestva pri plotnostyah, sootvetstvuyushih nedram neitronnyh zvezd s massami okolo 0.5 mass solnca. T.o. laboratornye i astrofizicheskie dannye mogut dopolnyat' drug druga. Uravnenie sostoyaniya-to v prirode dolzhno byt' odno! Chtoby ego vybrat' nuzhno brat' i dannye po otnositel'no massivnym neitronnym zvezdam, i dannye po svincu.
Authors: M. A. McLaughlin et al.
Comments: 5 pages, For Proceedings of the "Radio Pulsars" conference in Crete
Korotkaya zametka ob otkrytii novyh radiopul'sarov v skanah, provodimyh na teleskope v Aresibo. Udalos' otkryt' 10 novyh pul'sarov, u dvuh iz nih dovol'no korotkie perioda, no rekordov i sensacii net. Obrabotka dannyh prodolzhaetsya, i avtory nadeyatsya udvoit' chislo novyh ob'ektov.
Authors: R.X. Xu
Commets: 8 page and no figure, IAU Symposium No.214, or at http://vega.bac.pku.edu.cn/~rxxu/publications/index_P.htm
Prostoi obzor po kvarkovym zvezdam, gde vse dovol'nl ponyatno razlozheno po polochkam.
Authors: R.X. Xu (PKU)
Commets: 9 page and no figure, The 6th pacific rim conference on steller astrophysics -- a tribute to Helmut A. Abt, or at http://vega.bac.pku.edu.cn/~rxxu/publications/index_C.htm
"Golye" strannye zvezdy - odin teoreticheski vozmozhnyh iz variantov takih zvezd, kotorye ne obladayut koroi iz obychnogo veshestva. Magnitosfera takih zvezd zapolnena elektron-pozitronnoi plazmoi. Neposredstvenno na poverhnosti zvezdy sushestvuet ochen' sil'noe elektricheskoe pole. Nikakih spektral'nyh osobennostei v ee spektre izlucheniya ne budet (t.k. otsutstvuyut iony na poverhnosti).
Authors: G. Lugones, J. E. Horvath
Commets: 6 pages, 7 figures, Submitted to Astronomy & Astrophysics
"I na blohe sidit bloha". Sredi strannyh zvezd est' eshe bolee strannye. I esli strannye zvezdy kompaktnee neitronnyh, to "strannye strannye" zvezdy eshe bolee kompaktny. Rech' idet o t.n. color flavor locked (CFL) sostoyanii strannogo (kvarkovogo) veshestva. CFL-faza sootvetstvuet ravnomu chislu u, d, s kvarkov (nesmotrya na to, chto ih massy razlichny). Pri etom kvarki obrazuyut kuperovskie pary.
V stat'e avtory dayut obzor razlichnyh uravneniya sostoyaniya dlya takoi sredy, a takzhe rassmatrivayut strukturu sootvetstvuyushih kompaktnyh ob'ektov. Svoistva CFL-zvezd otlichny ot svoistv "obychnyh" strannyh zvezd. Naprimer, u CFL-zvezd, ne mozhet byt' kory iz normal'nogo veshestva, t.k. v nih net elektronov (chto privodit k otsutstviyu elektrostaticheskogo bar'era, meshayushgo obychnomu veshestvu peremeshat'sya s kvarkovym). T.o. CFL-zvezdy v chem-to pohozhi na "obnazhennye" kvarkovye zvezdy (sm. obozrenie za proshluyu nedelyu).
Authors: Bing Zhang
Commets: 8 pages, Invited talk at the Sixth Pacific Rim Conference on Stel Astrophysics, a tribute to Helmut A. Abt, July 11-17, 2002, Xi'an. To appear in the proceedings (eds. K. S. Cheng, K. C. Leung & T. P. Li)
Nedostayushim zvenom avtor schitaet otsutstvie pryamyh nablyudatel'nym svidetel'stv v pol'zu togo, chto chast' energetiki magnitarov ob'yasnyaetsya zamedleniem. Avtor podrobno razbiraet vozmozhnye istochniki energii magnitarov (istochnikov myagkih povtoryayushihsya gamma-vspleskov i anomamal'nyh rentgenovskih pul'sarov).
Stat'ya takzhe prosto yavlyaetsya horoshim kratkim opisanie togo, chto takoe istochniki myagkih povtoryayushihsya gamma-vspleskov i anomamal'nye rentgenovskie pul'sary.
Authors: A. Y. Potekhin, G. Chabrier
Commets: 23 pages, 12 figures, 1 table. AASTeX v.5.0 with emulateapj5.sty. Accepted for publication in the Astrophysical Journal
Ne mogu ne otmetit' stat'yu po atmosferam neitronnyh zvezd s sil'nym magnitnym polem. Odnako, dlya bolee populyarnogo izlozheniya mozhno prochest' ne bol'shuyu stat'yu, a bolee korotkii variant astro-ph/0212077.
Authors: Mallory S.E. Roberts
Commets: 4 pages, to appear in the proceedings of the conference "Radio Pulsars" held in Chania, Crete, Sept. 2002
Iz 270 istochnikov tret'ego kataloga EGRET dve treti ne otozhdestvleny. Nekotorye iz nih mogut byt' vnegalakticheskimi (blazary), no bol'shinstvo demonstriruet koncentraciyu v ploskosti Galaktiki. Mozhet byt' eto odinochnye chernye dyry. Vozmozhno, eto neitronnye zvezdy. Eto mogut byt' kak sovsem molodye ob'ekty (naprimer, rozhdennye v Poyase Gulda), tak i nemnogo bolee starye radiopul'sary, chei puchok ne popadaet na Zemlyu (po etoi tematike v mae budet zamechatel'naya konferernciya v Gonkonge). Avtor rasskazyvaet o vedushihsya poiskah radiopul'sarov sredi ob'ektov EGRET.
Authors: Bryan Gaensler
Commets: 10 pages, 3 embedded EPS figures, 3 JPG figures, uses cospar.sty. Invited review to appear in "High Energy Studies of Supernova Remnants and Neutron Stars" (COSPAR 2002), Advances in Space Research, in press. PS version with all figures embedded available at http://cfa-www.harvard.edu/~bgaensler/preprints/0212086.ps
Anomal'nye rentgenovskie pul'sary (ARP) i istochniki myagkih povtoryayushihsya gamma-vspleskov (MPG) po vsei vidimosti yavlyayutsya molodymi odinochnymi sil'nozamagnichennymi neitronnymi zvezdami. Znachit, mozhno ozhidat', chto oni budut nahodit'sya vnutri ili v neposredstvennoi blizosti ostatkov sverhnovyh. Odnako, tut ne vse tak prosto. Rasstoyaniya izmeryayutsya ne ochen' horosho, vozrasta - eshe huzhe. My vse vidim v proekcii na nebesnuyu sferu. A potomu v kazhdom konkretnom sluchae vopros o real'nosti svyazi mezhdu neitronnoi zvezdoi i ostatkom sverhnovoi trebuet podrobnogo razbiratel'stva (i vse ravno zachastuyu ostayutsya somneniya). V nebol'shom obzore avtor detal'no razbiraet etu problemu. Po vsei vidimosti ARP yavno pokazyvayut svyaz' s ostatkami, a vot MPG - net. Avtor vyskazyvaet gipotezu, chto eto mozhet byt' svyazano s tem, chto poslednie obrazovalis' v rezul'tate vzryvov bolee massivnyh zvezd.
Authors: Shou-Guan Wang, Zong-Hong Zhu, Zhen-Long Zou, Yuan-Zhong Zhang
Commets: 5 pages, no figure, Latex file Journal-ref: Int.J.Mod.Phys. D11 (2002) 1061-1065
Davno izvestna ideya ispol'zovat' pul'sary dlya registracii sverhnizkochastotnyh gravitacionnyh voln s periodami ot 1 do 100 let. Teper' dlya etoi zadachi predlagaetsya postroit' special'nyi 50 m radioteleskop, kotoryi budet regulyarno izmeryat' taiming 10 naibolee stabil'nyh millisekundnyh pul'sarov.
Authors: Anatoly A. Svidzinsky
Commets: 43 pages, 7 figures, to appear in Astrophysical Journal
Kogda govoryat ob izluchenii neitronnyh zvezd, obychno rassmatrivayut elektromagnitnoe (teplovoe) izluchenie s poverhnosti i izluchenie neitrino iz centra neitronnyh zvezd. V dannoi stat'e rassmotren eshe odin mehanizm perenosa energii - besstolknovitel'nyi elektronnyi zvuk. Zvukovye vozmusheniya v elektronnoi komponente neitronnoi zvezdy rasprostranyayutsya po nei stol' zhe svobodno, kak i neitrino. Istochnikom takih zvukovyh vozbuzhdenii sluzhat vihrevye niti v sverhtekuchem vrashayushemsya yadre. Pri nalichii magnitnogo polya elektronnyi zvuk mozhet prevrashat'sya v magnitozvukovye volny, kotorye vblizi poverhnosti prevrashayutsya v elektromagnitnoe izluchenie.
Authors: K.D.Kokkotas et al.
Commets: 4 pages, 2 figures
Rech' idet o neitronnyh (kvarkovyh i t.p) zvezdah, chei radius ne prevoshodit tri shvarcshil'dovskih. V etom sluchae vokrug zvezdy obrazuetsya (kak vokrug chernoi dyry) ergosfera. Takaya situaciya mozhet soprovozhdat'sya vozniknoveniem ves'ma specificheskoi neustoichivosti (w-mode instability). Eto sobstvenno neustoichivost' prostranstva-vremeni. Avtory rassmatrivayut vozmozhnost' voniknoveniya neustoichivosti v real'noi astrofizicheskoi situacii, a takzhe obsuzhdayut astrofizicheskie proyavleniya.
Authors: Tania Regimbau, Jose Antonio de Freitas Pacheco
Commets: 5 pages, 3 figures accepted for publication in Astronomy & Astrophysics
Buduchi nemnogo deformirovannymi ob'ektami vrashayushiesya neitronnye zvezdy yavlyayutsya istochnikami gravitacionnyh voln. Uzhe davno provodyatsya popytki rasschitat', chto smogut uvidet' detektory tipa VIRGO i LIGO ot takih ob'ektov. V svoei rabote avtory ispol'zuyut sobstvennuyu model' populyacionnogo sinteza radiopul'sarov dlya predskazanii grav. signala ot nih.
Authors: V.V.Gvaramadze
Commets: 4 pages, to appear in High Energy Processes and Phenomena in Astrophysics, Proceedings of IAU Symposium #214, held 5-10 August 2002 in Suzhou, China. Edited by Xiangdong Li and Virginia Trimble
Neitronnye zvezdy obrazuyutsya posle vzryvov sverhnovyh. No pochemu-to v ostatkah my vidim ne tak uzh mnogo radiopul'sarov. Vozmozhno, prosto daleko ne vse neitronnye zvezdy v svoei molodosti prohodyat cherez etu stadiyu. No est' eshe odna vozmozhnost'. Prosto my hotim naiti pul'sar v centre ostatka, inache my govorim, chto trebuetsya slishkom bol'shaya skorost', chtoby ob'yasnit' bol'shoe smeshenie neitronnoi zvezdy ot centra ostatka, i schitaem associaciyu rezul'tatom sluchainoi proekcii radiopul'sara na ostatok sverhnovoi. V etoi korotkoi zametke avtor summiruet rezul'taty issledovanii, kotorye pytayutsya uchest', chto iznachal'no neitronnaya zvezda mozhet byt' ne v centre ostatka. Priyaina ochen' prosta. Poka massivnyaya zvezda eshe zhivet, ona proizvodit moshnyi zvezdnyi veter, vyduvaya polost', no pri etom ona eshe i dvizhetsya. Poetomu vzryv mozhet proizoiti vnutri dovol'no slozhnoi struktury, prichem ne v ee centre.
Authors: Alfredo B. Henriques and Luis E. Mendes
Commets: 8 pages
My horosho znaem fermionnye zvezdy - k nim otnosyatsya belye karliki, neitronnye i, poka gipoteticheskie, kvarkovye zvezdy. Bolee dvadcati let nazad byla razrabotana teoriya bozonnyh zvezd - sostoyashih iz tak i ne otkrytyh do segodnyashnego dnya skalyarnyh chastic. No okazyvaetsya est' i smeshannye bozonno-fermionnye konstrukcii, kotorye nastol'ko gibki, chto pozvolyayut s pomosh'yu odnoi modeli ob'yasnit' ogromny ryad yavlenii - ot ob'ektov s atomnymi razmerami i massoi 1018 g, do ob'ektov s galakticheskimi massami, v kotoryh nebol'shoe yadro okruzheno protyazhennoi obolochkoi.
Na segodnya eta model' - skoree igra uma, no vdrug zavtra kto-to Obnaruzhit takuyu zvezdu (ili galaktiku:?)
Authors: P. Haensel
Commets: 35 pages, 11 figures, uses eas.cls, to be published in `Final Stages of Stellar Evolution'', edts. J.-M. Hameury and C. Motch, EAS Publications Series (EDP Sciences, 2003)
Teoretikov mnogo, a priroda odna.... Uravnenie sostoyaniya dolzhno byt' edinstvennym, no poka net dostatochno detal'nyh nablyudatel'nyh dannyh. A potomu sushestvuet mnozhestvo modelei, o kotoryh i rasskazyvaetsya v stat'e.
Authors: F.P. Gavriil, V.M. Kaspi, P.M. Woods
Commets: 10 pages, 7 figures, to appear in the proceedings of the 34th Cospar Scientific Assembly
Avtory dayut obzor svoih nablyudenii i obrabotki arhivnyh dannyh po anomal'nym rentgenovskim pul'saram. Osoboe vnimanie udeleno povedeniyu proizvodnoi perioda na bol'shih vremennyh otrezkah, a takzhe vspyshkam v rentgenovskom diapazone (kotorye rodnyat ARP s MPG).
Authors: M. Kramer (Manchester University, Jodrell Bank), O. Loehmer, A. Karastergiou (MPIfR Bonn)
Commets: 4 pages,to appear in "Radio Pulsars" (ASP Conf. Ser.), eds. M. Bailes, D. Nice, & S. Thorsett
V ochen' korotkoi stat'e sobrany sovremennye dannye po geodezicheskoi precessii neitronnoi zvezdy (precessii v iskrivlennom tyagoteniem prostranstve-vremeni) v Hals-Teilorovskom dvoinom pul'sare (eta sistema byla otkryta pervoi i nablyudaetsya dol'she vseh ostal'nyh).
Authors: Kaya Mori, Charles J. Hailey
Commets: 26 pages, 8 figures, submitted to ApJ
U neitronnoi zvezdy 1E1207.4-5209 po dannym Chandry obnaruzheno dve shirokie spektral'nye detali. Avtory stat'i dayut interpretaciyu etim nablyudeniyam. Po ih raschetam za detali otvetstvenny geliepodobnye atomy kisloroda v magnitnom pole 1012 Gs (tipichnom dlya neitronnyh zvezd). Esli schitat', chto massa neitronnoi zvezdy primerno 1.4 massy Solnca, to mozhno sdelat' ogranicheniya na uravneniya sostoyaniya: ono okazyvaetsya dostatochno zhestkim.
Authors: F.Graham Smith, C. Jordan
Commets: 6 pages 5 figures, to appear in "Radio Pulsars" (ASP Conf. Ser.), eds. M. Bailes, D. Nice, & S. Thorsett
Za 33 goda nablyudenii pul'sara v Krabe nablyudalos' 14 glitchei (sboev perioda vrasheniya), za kotorymi shli periody relaksacii. No vse eti sboi mozhno predstavit' kak 3 "gigantskih" sobytiya razdelennyh primerno 12 godami. Takaya gipoteza pozvolyaet snyat' nekotorye problemy s zakonami tormozheniya.
Authors: H. Quaintrell et al.
Commets: Accepted for publication in Astronomy & Astrophysics, 12 pages
Opredelenie mass neitronnyh zvezd - ochen' vazhnaya zadacha, t.k. ona napryamuyu svyazana s fizikoi povedeniya veshestva pri ekstremal'nyh plotnostyah. Poka horosho opredeleny massy u neskol'kih radiopul'sarov. Voobshe, massy v astronomii proshe opredelyat' v dvoinyh sistemah. Poetomu, krome dvoinyh radiopul'sarov, bol'shoe vnimanie privlekayut rentgenovskie pul'sary. Ih izvestno neskol'ko desyatkov. No v formulu dlya opredeleniya massy vhodyat parametry orientacii orbity, kotorye obychno neizvestny. Krome sluchaev zatmennyh sistem. Nalichie zatmenii oznachaet, chto my nahodimsya pochti p ploskosti orbity. Dlya takih sistem, esli est' dannye po spektroskopii normal'noi zvezdy, mozhno dovol'no tochno opredelit' massu neitronnoi. Izvestno 7 rentgenovskih pul'sarov s zatmeniyami. Vela X-1 - odin iz nih.
Dolgoe vremya massa neitronnoi zvezdy v Vela X-1 byla samoi vysokoi (1.9 mass Solnca, Barziv i dr. 2001) i potomu s etim rezul'tatom sporili. I vot nezavisimaya gruppa podtverzhdaet vysokuyu massu neitronnoi zvezdy! Uchityvaya vse neopredelennosti massa sostavlyaet ot 1. 75 massy Solnca do 2. 44.
O drugih, menee tochnyh, sposobah ocenki massy i ogranicheniyah na uravnenie sostoyaniya sm. svezhuyu rabotu "X-ray Studies of Two Neutron Stars in 47 Tucanae: Toward Constraints on the Equation of State" astro-ph/0301235 i vyshe astro-ph/0301161. Proizvedeny, takzhe, izmereniya v sisteme J1740-5340, gde millimekundnyi pul'sar isparyaet malomassivnogo soseda (astro-ph/0301244). Polucheno horoshee znacheniya dlya otnosheniya mass komponentov, no sami massy oceneny s bol'shoi oshibkoi.
Authors: D.R. Lorimer
Commets: 10 pages, 5 figures, to appear in the proceedings of the workshop "Pulsars, AXPs and SGRs observed with BeppoSAX and other Observatories" held in Marsala, Sicily, September 2001
Daetsya ponyatnyi obzor po svoistvam molodyh radiopul'sarov i po nedavnim otkrytiyam v etoi oblasti. Rassmatrivayutsya associacii pul'sarov s ostatkami sverhnovyh, a takzhe vozmozhnye otozhdestvleniya s gamma-istochnikami sputnika EGRET.
Authors: Simon Vidrih et al.
Commets: 4 pages, 3 figures.
Osnovoi etoi stat'i posluzhili 8 let stroboskopicheskih (s periodom 0.033 c) nablyudenii pul'sara v Krabovidnoi tumannosti. Fur'e analiz pokazal znachimoe prisutstvie 60-sekundnoi modulyacii signala, kotoruyu avtory interpretiruyut kak svobodnuyu precessiyu pul'sara.
Authors: Matthias Stute, Max Camenzind
Commets: Comments: 11 pages, 18 figures, accepted for publication in MNRAS
Journal-ref: MNRAS 336, 831 (2002)
Nalichie poverhnosti i bystroe vrashenie neitronnyh zvezd delaet neprimenimymi dlya rascheta akkrecii na nih resheniya, poluchennye dlya chernyh dyr. V 2000 g. Manko i dr. udalos' poluchit' reshenie uravnenii Einshteina, horosho opisyvayushee pole vne neitronnoi zvezdy. Odnako, massa, uglovoi moment i kvadrupol'nyi moment, vhodyashie v uravnenie, dlya real'nyh neitronnyh zvezd svyazany drug s drugom (kvadrupol'nyi moment opredelyaetsya massoi i vrasheniem). Eto tozhe nuzhno kak-to uchityvat'. Dlya etogo provodilis' chislennye vychisleniya (Kuk i dr. 1994). Shtute i Kamenzind v svoei stat'e pytayutsya ob'edinit' dva podhoda (Manko i dr. i Kuka i dr.) dlya polucheniya samosoglasovannoi relyativistskoi modeli gravitacionnogo polya vne neitronnoi zvezdy (pohozhii podhod, no bez primeneniya novogo resheniya Manko i dr. primenyalsya v rabotah Sibgatullina i Syunyaeva).
Authors: Roger W. Romani, C.-Y. Ng
Commets: 4 pages, 4 figures, to appear in the Astrophysical Journal Letters
V fizike neitronnyh zvezd temnym poka ostaetsya vopros o korrelyacii razlichnyh parametrov etih ob'ektov, a takzhe vopros o proishozhdenii vysokih prostranstvennyh skorostei (konechno, etim spisok "tain i zagadok" ne ogranichivaetsya!). V dannoi stat'e opisyvayutsya novye nablyudatel'nye dannye po pul'saru PSR J0538+2817, a takzhe privodyatsya vozmozhnye sledstviya iz etih dannyh.
Krome togo, chto est' osnovaniya polagat', chto nachal'nyi period vrasheniya etoi neitronnoi zvezdy byl dovol'no bol'shim (bolee 130 millisekund), dannye nablyudenii pozvolyayut sdelat' vazhnye ogranicheniya na scenarii priobreteniya zvezdoi prostranstvennoi skorosti. Delo v tom, chto u etogo ob'ekta, kak i u neskol'kih drugih, otkryt tor. Schitaya, chto vektor vrasheniya zvezdy sovpadaet s vektorom vrasheniya tora, mozhno opredelit' ugol mezhdu vektorom prostranstvennoi skorosti i vektorom vrasheniya. V predelah oshibok etot ugol raven 0 (kak i u Kraba i Vely). Sama skorost' pul'sara nevelika - poryadka 140 km/s. Daleko ne vse scenarii dayut skorost' vdol' osi vrasheniya! Krome togo, nado ob'yasnyat' bol'shoi period i malyi modul' skorosti...
Authors: Tod Strohmayer, Lars Bildsten
Commets: 45 pages, 17 figures. To appear in Compact Stellar X-Ray Sources, eds. W.H.G. Lewin and M. van der Klis, Cambridge University Press
Termoyadernye vspyshki na neitronnyh zvezdah i belyh karlikah izvestny dovol'no davno (po merkam razvitiya nauki). Odnako, zapusk vse novyh i novyh rentgenovsih sputnikov prinosit vse novye i novye dannye. V tom chisle otkryvayutsya dosele neizvestnye yavleniya. Imenno teoreticheskomu osmysleniyu etih novyh otkrytii i posvyashen obzor.
Authors: Simon DeDeo, Dimitrios Psaltis
Commets: 4 pages, 4 figures. Accepted to Physical Review Letters
Pokazano, kak dannye po spektroskopii neitronnyh zvezd mogut pomoch' v "ubienii" teorii gravitacii, proshedshih proverku v Solnechnoi sisteme (vsem al'ternativshikam - prochest' i primenit' na praktike!).
Authors: Robert E. Rutledge et al.
Commets: 43 pages, ApJ, submitted
Ne mogu uderzhat'sya ot upominaniya ochen' vazhnoi raboty dlya oblasti, v kotoroi
ya rabotayu.
Opisyvaetsya poisk novyh kandidatov v odinochnye neitronnye zvezdy.
Vrode by poluchennye rezul'taty nahodyatsya v sootvetstvii s nashimi poslednimi
predskazaniyami. Uff....
Authors: K.J. Pearson, Keith Horne, Warren Skidmore
Commets: 14 pages, 5 figures, Review of propeller systems to appear in the proceedings of Magnetic Cataclysmic Variables IAU Coll. 190, eds. M. Cropper, S. Vreilmann
V evolyucii zamagnichennyh kompaktnyh ob'ektov (neitronnyh zvezd i belyh karlikov) est' takaya interesnaya stadiya - Propeller.
Pro neitronnye zvezdy na etoi stadii izvestno ne ochen' mnogoe (a hotelos'
by!). Vozmozhno, dannyh po belym karlikam bol'she. Ob etom i rasskazyvaetsya v
dannom obzore. Stadiya eta neprostaya. Tradicionno priglashaem fizikov plazmy
obratit' na nee svoe vnimanie.
Authors: Dong Lai, W.C.G. Ho
Commets: 10 pages with 5 figures. To appear in "High Energy Processes and Phenomena in Astrophysics, IAU Symposium 214, X. Li, Z. Wang, V. Trimble (eds)
Est' izvestnaya situaciya: iz goda v god na raznyh konferenciyah odni i te zhe lyudi delayut doklady na odni i te zhe ("svoi") temy. Kak raz takoi sluchai. Ho i Lai yavlyayutsya izvestnymi specialistami po neitronnym zvezdam voobshe i po fizike veshestva v sil'nym magnitnyh polyah v chastnosti. Vot ih ocherednoi obzor. V svyazi s rostom chisla nablyudenii i teoreticheskih raschetov poyavlenie novyh obzorov vyglyadit vpolne opravdannym.
Authors: Jun Yokogawa et al.
Commets: 61 pages, 19 figures, to be published in PASJ. Also available at http://www-cr.scphys.kyoto-u.ac.jp/member/jun/job/ (with high-resolution images)
Sputnik ASCA mnogo nablyudal MMO. Vsego bylo zaregistrirovano 106 istochnikov (sredi nih tesnye dvoinye, ostatki sverhnovyh i dr.). V stat'e daetsya obzor i analiz etih dannyh.
- astro-ph/0302301
Modelirovanie slivayushihsya neitronnyh zvezd s vysokim razresheniem: izluchenie neitrino (High Resolution Calculations of Merging Neutron Stars II: Neutrino Emission)
Authors: S. Rosswog, M. Liebendoerfer
Commets: 39 pages, 13 figures, submitted to MNRAS; Movies can be found under http://www.astro.le.ac.uk/~sro/movies.html, higher quality figures under http://www.astro.le.ac.uk/~sro/publications.html
- astro-ph/0302313
Inercial'nye mody neitronnyh zvezd so sverhtekuchimi yadrami (Inertial modes of neutron stars with the superfluid core)
Authors: Shijun Yoshida, Umin Lee
Commets: 18 pages, 20 figures
- astro-ph/0302314
Akkrecionnyi disk i ego vyzhivanie v techenie razrusheniya neitronnoi zvezdy chernoi dyroi (Accretion disk assembly and survival during the disruption of a neutron star by a black hole)
Authors: Enrico Ramirez-Ruiz, William H. Lee
Commets: 4 pages, 2 figures, to appear in the proceedings of the Rome 2002 GRB workshop
- gr-qc/0301112
K voprosu o realistichnom "vspiralivanii" dvoinyh neitronnyh zvezd (Towards a Realistic Neutron Star Binary Inspiral)
Authors: Mark Miller, Wai-Mo Suen
Commets: 4 pages, 3 figures, revtex4
- astro-ph/0302332
Otdacha, perpendikulyarnaya vrasheniyu, ...
(Spin-perpendicular kicks from evanescent binaries formed in the
aftermath of rotational core-collapse and the nature of the observed
bimodal
distribution of pulsar peculiar velocities)
Authors: Monica Colpi, Ira Wasserman
Commets: To appear in the proceedings of the International Workshop on "Pulsars, AXPs, and SGRs observed with BeppoSAX and other Observatories" (Marsala, Sicily, 23-25 September 2002); 6 pages, 1 figure
Srazu neskol'ko rabot raznyh avtorov po slivayushimsya kompaktnym ob'ektam. Pervaya i tret'ya stat'i posvyasheny chislennym raschetam sliyanii. Vo vtoroi stat'e spiska rassmatrivaetsya vnutrennee stroenie neitronnyh zved. V chetvertoi - izuchayutsya nekotorye teorfizicheskie aspekty sliyanii. V pyatoi avtory pytayutsya ob'yasnit' bimodal'nost' raspredeleniya nachal'nyh skorost neitronnyh zvezd raznymi mehanizmami priobreteniya skorosti.
Authors: D. L. Kaplan, S. R. Kulkarni, M. H. van Kerkwijk
Commets: 5 pages, 4 figures. Uses emulateapj5.sty, onecolfloat5.sty. Submitted to ApJL
Otozhdestvlenie bylo, konechno, proizvedeno na Habblovskom teleskope. Zvezdnaya velichina ob'ekta 26.8, on ochen' goluboi i lezhit vnutri boksov oshibok HRI i Chandra. Veroyatno my vidim Relei-Dzhinsovskuyu chast' teplovogo spektra. Eti nablyudeniya podtverzhdayut, chto istochnik RX J1605.3+3249 - odinochnaya neitronnaya zvezda.
Authors: R. Dodson, D. Legge, J.E. Reynolds, P.M. McCulloch
Commets: submitted to ApJ
mu(alpha cos delta)=-49.60+/-0.06 m"/god, mu(delta)=+29.8+/-0.1 m"/god, parallaks p=3.4+/-0.2 m".
Authors: Bennett Link (Montana State University)
Commets: 10 pages, 1 figure
Standartnaya kartinka, v kotoroi v yadre neitronnoi zvezdy sverhtekuchimi yavlyayutsya kak neitrony, tak i protony, protivorechit nablyudaemoi dolgoperiodicheskoi (~1 god) precessii neitronnyh zvezd. Libo tol'ko odna iz ukazannyh komponent yavlyaetsya sverhtekuchei, libo "chasti" yadra sil'no svyazany magnitnym polem.
Authors: F. Haberl
Commets: COSPAR Symposium on High Energy Studies of Supernova Remnants and Neutron Stars, Houston, Oct. 2002
Obzor rezul'tatov s Chandry i HMM-N'yutona po odinochnym neitronnym zvezdam: ob'ektam "velikolepnoi semerki" i anomal'nym rentgenovskim pul'saram.
Authors: A. Krawczyk et al.
Commets: 11 pages, 11 figures, to appear in MNRAS
K nastoyashemu momentu byli dannye o 76 glitchah (sboyah perioda) ot 25 pul'sarov. V dannoi stat'e predstavleny rezul'taty novyh nablyudenii. Avtory soobshayut o 14 glitchah ot 9 pul'sarov (6 iz nih "sboinuli" vpervye). Eti dannye ochen' vazhny dlya ponimaniya prirody neitronnyh zvezd voobshe i radiopul'sarov v chastnosti (naprimer, mozhno pytat'sya "vytyanut'" dannye o mehanicheskih svoistvah kory i yadra, a takzhe o svyazi mezhdu nimi).
Authors: B.P. Gong
U vse bol'shego chisla pul'sarov nablyudaetsya vekovaya peremennost'. V chastnosti menyayutsya proekciya poluosi na luch zreniya, proizvodnaya orbital'nogo perioda, prichem eti izmeneniya na neskol'ko poryadkov velichiny vyshe, chem vyzyvaemye effektami OTO. Togda eti dannye pozvolyayut ocenit' moment inercii neitronnoi zvezdy - ot 1044 g.sm2 do 1045 g.sm2.
Authors: D. L. Kaplan et al.
Commets: 13 pages, 9 figures. Uses emulateapj5.sty and onecolfloat5.sty. Accepted for publication in ApJ
Vse, chto my znaem, ob odnoi iz blizhaishih radiotihih neitronnyh zvezd - odnoi iz "velikolepnoi semerki".
Authors: E. V. Gotthelf
Commets: 6 pages, 3 figures, 1 table, LaTex, emulateapj5.sty. To appear in the June 20, 2003 issue of the Astrophysical Journal
Novye nablyudeniya trebuyut utochnenii modelei. Dannye Chandry, pozvolivshie podrobno izuchit' 9 krabopodobnyh pul'sarov i ih tumannosti, trebuyut peresmotra modeli rentgenovskih spektrov etih ob'ektov. Vo mnogom eto svyazano s tem, chto predydushie nablyudeniya ne mogli razdelit' spektry samogo pul'sara i tumannosti (iz-za nizkogo uglovogo razresheniya). V stat'e predstavleny rezul'taty popytki postroeniya novoi fenomenologicheskoi modeli.
Authors: J. G. Kirk and O. Skjaeraasen
Commets: Accepted for publication in ApJ
Vnutri svetovogo cilindra energiya vrasheniya pul'sara perenositsya prakticheski polnost'yu elektromagnitnym potokom (potokom Pointinga), eto vyvod vseh sovremenny teorii i modelei. A uzhe nedaleko za svetovym cilindrom eta energiya prakticheski polnost'yu okazyvaetsya zaklyuchennoi v potoke relyativistskih chastic (vzaimodeistvie kotoryh s veshestvom nablyudaetsya). Raspredelenie unosimoi energii mezhdu elektromagnitnym potokom i chasticami opisyvaetsya parametrom sigma. Polnoi modeli dannogo processa na segodnyashnii den' net.
Authors: G.J. Qiao, K.J. Lee, H.G. Wang, R.X. Xu
Commets: 4 pages, 1 figure, in the meeting on "Radio Pulsars", Crete 2002, in press
Nesmotrya na to, chto pul'sary izvestny uzhe bolee 35 let, mehanizm ih izlucheniya do konca ne ponyat. Avtory stat'i predstavlyayut ocherednuyu popytku opisat' izluchenie pul'sarov ot radio do gamma diapazona v edinoi modeli.
Dannaya stat'ya - eto materialy konferencii. potomu tut ochen' kratko, tezisno, perechisleny osnovnye cherty modeli. Osnovnuyu rol' v podhode avtorov stat'i igraet obratnoe komptonovskoe rasseyanie. Podgonkoi parametrov modeli im udaetsya opisat' impul'sy 7 horosho izuchennyh pul'sarov.
Authors: Igor A. Shovkovy, Paul J. Ellis
Commets: 7 pages. Talk presented at 2002 International Workshop "On Strong Coupling Gauge Theories And Effective Field Theories" (SCGT 02), 10-13 December 2002, Nagoya, Japan
V fizike neitronnyh zvezd ochen' vazhnoi i interesnoi zadachei yavlyaetsya raschet ih ohlazhdeniya. Delo v tom, chto s odnoi storony eta problema trebuet ponimaniya povedeniya veshestva v ekstremal'nyh usloviyah, s drugoi - eto mozhno proverit' v nablyudeniyah (sm., naprimer, raboty Sankt-Peterburgskoi gruppy i ih obzor v UFN).
T.n. "strannye zvezdy" ohlazhdayutsya po-drugomu.... Ob etom avtory rasskazyvayut v obsuzhdaemoi stat'e. Eto ne obzor, odnako, mnogie vazhnye ssylki prisutstvuyut. Krome togo v statei "mnogo fiziki, malo formul". T.o. eta korotkaya zametka budet interesna fizikam.
Authors: M. Revnivtsev et al. (MPA, Garching, Germany; IKI, Moscow, Russia)
Commets: Accepted for publication in Astronomy Letters
Eto odna iz pervyh otechestvennyh statei (a mozhet byt' prosto pervaya), napisannaya po dannym zapushennogo v konce 2002 gody sputnika INTEGRAL. Zhestkii rentgenovskii IGR J16318-4848 otkryt s INTEGRALa, zatem ego udalos' obnaruzhit' v arhivnyh dannyh yaponskogo sputnika ASCA (1994), no tam on ne byl identificirovan. Istochnik obladaet sovershenno neobychnymi svoistvami - pohozhe on svetit cherez tolstyi sloi veshestva - ranee takogo nigde ne nablyudalos'. Pervaya predlozhennaya model' - akkreciruyushii iz zvezdnogo vetra istochnik v massivnoi dvoinoi sisteme.
Authors: D. Eichler, Y. Lyubarsky, C. Thompson, P.Woods
Commets: 8 pages, 1 fig. To appear in Proc. Marsala workshop "Pulsars, AXPs and SGRs observed with BeppoSAX and other observatories"
"V mire skazok tozhe est' bulochki". U istochnikov myagkih povtoryayushihsya gamma-vspleskov tozhe est' rentgenovskie poslesvecheniya. Avtory pokazyvayut, kak etot fenomen nahodit svoe ob'yasnenie v ramkah naibolee populyarnyi na segodnyashnii den' magnitarnoi gipotezy.
Authors: Andrej Cadez et al.
Commets: 6 pages, 7 figures. Published in A&A Journal-ref: 2001 A&A, 366, 930C
O predvaritel'nyh rezul'tatah etogo eksperimenta soobshalos' v preprinte astro-ph/0301328. Bolee dlinnyi ryad sinhronnyh s osevym vrasheniem opticheskih nablyudenii pul'sara v Krabe po prezhnemu podtverzhdaet nalichie perioda 60 s, kotoryi interpretiruetsya kak svobodnaya precessiya.
No v etih dannyh poyavilsya novyi sushestvennyi argument v pol'zu togo, chto eto precessiya - ee period zamedlyaetsya primerno v tom zhe tempe, v kakom izmenyaetsya period vrasheniya samogo pul'sara, kak i dolzhno byt' pri svobodnoi precessii!
Authors: Katherine E. McGowan et al.
Commets: 24 pages, 6 figures, 3 tables, accepted for publication in ApJ
XMM-N'yuton vpervye zaregistriroval pul'siruyushee rentgenovskoe izluchenie ot 143 ms pul'sara PSR J0538+2817. Spektr etogo izlucheniya - chernotel'nyi s temperaturoi Tinfty = (2.12 +0.04/-0.03) x 106 K, a radius izluchayushei oblasti - 0.70+/-0.02 km, t.e. svetit nagretaya polyarnaya shapka.
Authors: Bryan M. Gaensler
Commets: 8 pages, 4 embedded EPS figures, uses ws-procs9x6.cls. To appear in proceddings of "Texas in Tuscany" (XXI Symposium on Relativistic Astrophysics)
Korotkii obzor svezhih dannyh i idei po pul'saram i pul'sarnym vetram. Vozmozhno imenno pul'sarnye tumannosti smogut prolit' svet na vazhnye detali mehanizma raboty pul'sara. Po-krainei mere vo vsei etoi nauke poyavlyayutsya principial'no novye dannye, t.o. posle nekotorogo zastoya/zatish'ya pul'sarnaya mashina snova na perednem krayu astrofiziki.
Authors: Andreas Reisenegger, Axel Bonacic
Commets: 6 pages,3 figures, to be published in the conference proceeding of "International Workshop On Pulsars, AXPs And SGRs Observed With Bepposax And Other Obervatories", Marsala (Sicily, Italy), 23 - 25 September 2002
Obsuzhdaetsya rol' vyazkosti pri evolyucii molodoi neitronnoi zvezdy, v kotoroi vozbuzhdeny r-mody. Poslednie ispytali pristal'noe vnimanie teoretikov v poslednie neskol'ko let v svyazi s tem, chto, kak polagali, imenno oni mogli otvechat' za nachal'nye periody neitronnyh zvezd, a takzhe mogli by byt' nablyudaemy s pomosh'yu detektorov gravitacionnyh voln. Odnako, fizika processa okazalas' ochen' slozhnoi (my vse-taki ploho predstavlyaem, kak vnutri ustroeny neitronnye zvezdy). Poetomu entuziazm neskol'ko ugas, i nachalas' ser'eznaya rabota.
Authors: M. Kramer et al.
Commets: accepted for publication in MNRAS, 31 pages, 10 figures
Sama stat'ya zanimaet menee 8 stranic. Ostal'noe - tablicy, profili impul'sov
i t.d. Kartinki dovol'no interesnye i informativnye (imeetsya vvidu, chto dazhe
dlya nespecialistoov eto mozhet byt' interesno v plane obshego razvitiya).
Opisyvayutsya svoistva molodyh pul'sarov (velopodobnye, t.e. pohozhie na
pul'sar v Vele - Parusah). Obsuzhdaetsya vozmozhnaya svyaz' molodyh pul'sarov s
neotozhdestvlennymi gamma-istochnikami sputnika EGRET.
Authors: I. A. Grenier
Commets: 8 pages, Proc. of the Texas Symposium, 2002, Florence, Italy
Sredi pochti treh soten istochnikov, zaregistrirovannyh priborom EGRET na Komptonovskoi observatorii (aka CGRO), otozhdestvleno menee 100. Ostal'nye zhdut svoego chasa. Tam, bezuslovno, est' i galakticheskie i vnegalakticheskie ob'ekty. Galakticheskie vydelyayutsya po svoemu raspredeleniyu (koncentraciya k ploskosti Galaktiki i t.d.). Imenno ih i rassmatrivaet v svoei stat'e Izabel' Gren'e. Osoboe vnimanie udelyaetsya neitronnym zvezdam iz Poyasa Gulda. O poslednem sm. takzhe stat'yu "3D dynamical evolution of the interstellar gas in the Gould Belt" astro-ph/0303516. V mae v Gong Konge budet celaya bol'shaya konferenciya po neotozhdestvlennym istochnikam EGRET. Nadeemsya, chto v nachale iyunya na Scientific.Ru poyavitsya rasskaz o nei.
astro-ph/0303582 Harakteristiki "shumovoi" variacii perioda pul'sara v Krabe (Characterization of the Crab Pulsar's Timing Noise)
Authors: D. Matthew Scott, Mark H. Finger, Colleen A. Wilson
Commets: 53 pages, 9 figures, submitted to MNRAS, abstract condensed
"Zhil na svete Zashibala.
Na "Minoge" on letal.
On otkryl planet nemalo,
I na kazhdoi zashibal."
(iz mul'tfil'ma "Vlastelin Vremeni")
"K chemu tut planety?"- sprosite vy. Chitaite.
Samye izvestnye neitronnye zvezdy - pul'sary. Samyi izvestnyi pul'sar - pul'sar v Krabovidnoi tumannosti. Period vrasheniya etoi neitronnoi zvezdy okolo 33 ms. Vspyshka sverhnovoi nablyudalas' v 1054 g.
V stat'e avtory rassmatrivayut izmeneniya perioda vrasheniya po dannym radionablyudenii. Krome zamedleniya perioda, krome vtoroi proizvodnoi, est' eshe "shumovye" variacii (timing noise). Avtory detal'no issleduyut etot "shum" (snova skazhu: vremya - prakticheski edinstvennoe, chto my tochno i model'no nezavisimo izmeryaem v astronomii, potomu nado vytyagivat' kak mozhno bol'she informacii). I tut my podhodim k samomu glavnomu.....
Obnaruzheny periodicheskie (kvaziperiodicheskie?) variacii na masshtabe 568+/-10 dnei. Ih mozhno ob'yasnyat' po-raznomu. Odno iz vozmozhnyh ob'yasnenii - planeta!
Planety u pul'sarov ne novost' ( sm. obzor). V 1992 g. v Nature poyavilas' stat'ya Wolszczan, A.; Frail, D. A. "A planetary system around the millisecond pulsar PSR1257 + 12". S teh por planety otkryvali (i zakryvali) ne raz. V nashei strane izvestnym ekspertom po pul'sarnym planetam yavlyaetsya Tat'yana Shabanova iz Pushino. Po vsei vidimosti, planety obrazuyutsya iz veshestva ostavshegosya posle vzryva sverhnovoi, odnako, tut eshe mnogo neyasnogo.
Esli u Kraba i pravda est' planeta, to ee massa kak minimum v 3 raza prevoshodit massu Zemli (voobshe, u pul'sarov otkryvayut planety s massoi, sravnimoi s zemnoi, a ne s yupiterianskoi).
My ne hotim sozdavat' vpechatlenie, chto "U PUL'SARA V KRABE OTKRYTA PLANETA!!!" I avtory stat'i ne hotyat. Nuzhny novye issledovaniya. No vozmozhnost' ochen' interesnaya.
Publikacii s klyuchevymi slovami:
astrofizika - obzory - ekzoplaneta - Planety u drugih zvezd
Publikacii so slovami: astrofizika - obzory - ekzoplaneta - Planety u drugih zvezd | |
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