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

Ostatki sverhnovyh
(Arhiv Ostatki sverhnovyh:
v.2, 2003, v.1, 2002-2003)

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

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).


Vypusk 186. 16-31 maya 2008

arxiv:0805.4557 Sverhnovaya, porodivshaya Kassiopeyu A, otnosilas' tipu IIB (The Cassiopeia A Supernova was of Type IIB)
Authors: Oliver Krause et al.
Comments: 17 pages, 4 figures, including online supporting material; to be published in Science on 30 May 2008

Ostatok sverhnovoi Kassiopeya A yavlyaetsya odnim iz samyh molodyh v Galaktike. V ego centre nablyudaetsya zagadochnyi kompaktnyi ob'ekt. Vse vremya idut spory o tom, k kakomu tipu otnosilas' sverhnovaya, porodivshaya ostatok i kompaktnyi ob'ekt.

Avtory analiziruyut opticheskii spektr, poluchennyi po nablyudeniyam svetovogo eha. Ideya sostoit v tom, chto my mozhet seichas nablyudat' otrazhenie samogo vzryva, i po spektru opredelit' tip sverhnovoi.

Analiz pokazal, chto vzorvalos' gelievoe yadro krasnogo giganta. T.e., sverhnovaya otnosilas' k tipu IIB.

Sm. takzhe arxiv:0805.4607, gde drugaya gruppa nablyudatelei takzhe privodit novyi dannye po ostatku Cas A.


Vypusk 181. 01-17 marta 2008 goda

arxiv:0803.1487 Samyi molodoi galakticheskii ostatok sverhnovoi: G1.9+0.3 (The Youngest Galactic Supernova Remnant: G1.9+0.3)
Authors: S.P. Reynolds, K.J. Borkowski, D.A. Green, U. Hwang, I. Harrus, R. Petre
Comments: 5 pages, 5 figures; submitted to ApJL

Avtory proveli detal'noe issledovanie ostatka sverhnovoi G1.9+0.3 na Chandre, a takzhe ispol'zovali dannye radionablyudenii. Itogom stal vyvod o tom, chto eto samyi molodoi iz izvestnyh galakticheskih ostatkov. Ego vozrast okolo 100 let. Ostatok nahoditsya v central'noi chasti Galaktiki. Pogloshenie tam veliko, tak chto sverhnovuyu vpolne mogli ne zametit'.

Kstati, o zvezdoobrazovanii v centre Galaktiki mozhno pochitat' zdes': arxiv:0803.1619.

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


Vypusk 179. 01-14 fevralya 2008 goda

arxiv:0802.0221 Infrakrasnoe eho razoblachaet vyhod udarnoi volny v sverhnovoi Kassipeya A (Infrared Echoes Reveal the Shock Breakout of the Cas a Supernova)
Authors: Eli Dwek, Richard G. Arendt
Comments: Submitted to The Astrophysical Journal - 31 pages including 12 figures

S odnoi storony, v stat'e ne soderzhitsya kakogo-to superotkrytiya. S drugoi - prosto interesno bylo razobrat'sya.

Neskol'ko let nazad po nablyudeniyam na kosmicheskoi infrakrasnoi observatorii imeni Spitcera bylo otkryto infrakrasnoe eho v ostatke sverhnovoi Kassiopeya A. Chto imeetsya v vidu? Imeetsya v vidu sleduyushee. Uvideli bystro peremeshayushiesya detali, kotorye srazu zhe identificirovali kak "solnechnye zaichiki". Central'naya vspyshka daet "bliki" na oblakah pyli (sobstvenno, v etih "zaichikah" my vidim teplovoe izluchenie pyli, do kotoroi doshlo zhestkoe izluchenie). Sut' yavleniya yasna, no inetersno zhe razorat'sya v tom, chto za izluchenie pereizluchaetsya.

V 2005 gody byla vyskazana gipoteza (ne prosto vyskazana, konechno, a podderzhana model'yu, nablyudeniyami, i opublikovana v Science) o tom, chto vspyshka proizoshla primerno v 1950 godu (napomnyu, chto samomu ostatku okolo 320 let. Zaodno ogovoryus', chto konechno vzryv sverhnovoi ne "proizoshel" 320 let nazad, a svet ot nego doshel do nas 320 let nazad, tozhe otnositsya i k drugim vremennym privyazkam). Gipoteza byla osnovana na analize dannyh ob IK eho. Sootvetstvenno, trebovalos', chtoby spustya pochti 300 let posle vspyshki sverhnovoi ostavshiisya kompaktnyi ob'ekt dal moshnuyu vspyshku (kstati, napomnyu, chto central'nyi kompaktnyi ob'ekt v etom ostatke dovol'no zagadochen. V rentgene nablyudaetsya nechto, chto s odnoi storony pohozhe na ostyvayushuyu neitronnuyu zvezdu, a s drugoi imeet ochen' malen'kuyu izluchayushuyu poverhnost' pri otsutstvii pul'sacii).

V novoi rabote avtory zanovo analiziruyut dannye po IK eho. Itogom raboty stalo zaklyuchenie o tom, chto vse mozhno ob'yasnit' bez vspyshki v 1950 godu. T.e., vse "zaichiki" porozhdeny fotonami, ispushennymi v moment vzryva sverhnovoi (tochnee, v moment vyhoda udarnoi volny iz zvezdy - otsyuda i zagolovok stat'i). Te "zaichiki", kotorye v proekcii vidny blizko k centru sverhnovoi prosto, po mneniyu avtorov, nahodyatsya "s toi storony" ostatka. Znachit, ne nado pridumyvat', chto sluchilos' v Kassiopee A 57 let nazad (a zhal', mozhno bylo krasivyi ogorod gorodit'. Naprimer, mog sluchitsya perehod kompaktnogo ob'ekta v kvarkovuyu zvezdu, chto zaodno ob'yasnyalo by i maluyu izluchayushuyu ploshad').


Vypusk 177. 10-21 yanvarya 2008 goda

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 175. 14-19 dekabrya 2007

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.


Vypusk 186. 16-31 maya 2008

arxiv:0805.4557 Sverhnovaya, porodivshaya Kassiopeyu A, otnosilas' tipu IIB (The Cassiopeia A Supernova was of Type IIB)
Authors: Oliver Krause et al.
Comments: 17 pages, 4 figures, including online supporting material; to be published in Science on 30 May 2008

Ostatok sverhnovoi Kassiopeya A yavlyaetsya odnim iz samyh molodyh v Galaktike. V ego centre nablyudaetsya zagadochnyi kompaktnyi ob'ekt. Vse vremya idut spory o tom, k kakomu tipu otnosilas' sverhnovaya, porodivshaya ostatok i kompaktnyi ob'ekt.

Avtory analiziruyut opticheskii spektr, poluchennyi po nablyudeniyam svetovogo eha. Ideya sostoit v tom, chto my mozhet seichas nablyudat' otrazhenie samogo vzryva, i po spektru opredelit' tip sverhnovoi.

Analiz pokazal, chto vzorvalos' gelievoe yadro krasnogo giganta. T.e., sverhnovaya otnosilas' k tipu IIB.

Sm. takzhe arxiv:0805.4607, gde drugaya gruppa nablyudatelei takzhe privodit novyi dannye po ostatku Cas A.


Vypusk 169. 19-30 sentyabrya 2007

item arxiv:0709.2880 Pyl', formiruyushayasya v ostatke sverhnovoi Kassiopeya A, po nablyudeniyam kosmicheskogo teleskopa Spitzer (Freshly Formed Dust in the Cassiopeia A Supernova Remnant as Revealed by the Spitzer Space Telescope)
Authors: J. Rho et al.
Comments: 28 pages, ApJ

Nedavnie otkrytiya bol'shogo kolichestva pyli (108 - 109 mass Solnca) v galaktikah i kvazarah na bol'shih krasnyh smesheniyah govoryat o tom, chto imenno sverhnovye vtorogo tipa SNe II yavlyayutsya effektivnym istochnikom pyli v rannei Vselennoi. Rezul'taty raschetov formirovaniya pyli pri vzryvah sverhnovyh SNe II (Todini, Ferrara, 2001; Nozawa et al 2003) podtverzhdayut etot fakt, predskazyvaya, chto odna SN II mozhet proizvodit' ot 0.1 do 1.0 mass Solnca pyli. Tem ne menee nablyudeniya blizkih ostatkov sverhnovyh do sih por byli bolee chem pessimistichny, davaya verhnii predel pylevoi massy na dva poryadka men'she predskazannogo. Kassiopeya A (Cas A) - molodoi ostatok galakticheskoi sverhnovoi vozrastom 335 let. V stat'e privedeny rezul'taty nablyudenii Cas A s pomosh'yu infrakrasnogo spektrografa na bortu Spitzer na dlinah voln ot 5.5 - 70 mkm. Po ocenkam avtorov, massa pyli v Cas A sostavlyaet ot 0.020 do 0.054 mass Solnca. Eto v desyat' raz men'she znacheniya, predskazannogo teoriei, no zato v desyat' raz bol'she predydushih ocenok 3.5 10-3 mass Solnca i 7.7 10-5 mass solnca. Takoi rezul'tat ne sluchaen. Vo-pervyh, v dannoi rabote infrakrasnyi spektr Cas A analizirovalsya vplot' do 70 mkm, togda kak avtory predydushih rabot ostanavlivalis' na 30-40 mkm. Vo-vtoryh, infrakrasnyi spektrograf (IRS) teleskopa Spitzer imeet bol'shoe razreshenie, i dlya togo, chtoby vosproizvesti v raschetah nablyudaemyi spektr potrebovalos' znachitel'no uslozhnit' model', vklyuchiv v nee pylevye chasticy raznogo himicheskogo sostava. Poskol'ku nablyudeniya velis' tol'ko do 70 mkm, v dannoi rabote ne uchtena holodnaya pyl' Cas A, eto odna iz vozmozhnyh prichin raznoglasiya s teoreticheskim znacheniem. No otvetit' na etot vopros pozvolyat tol'ko budushie infrakrasnye i submillimetrovye nablyudeniya s pomosh'yu teleskopov Herschel, SCUBA-2 i ALMA. Vazhno otmetit', chto kolichestvo pyli, formiruyusheesya v ostatke sverhnovoi, est' funkciya massy i metallichnosti zvezdy. A temp sverhnovyh (kolichestvo sverhnovyh, vzryvayushihsya v edinicu vremeni) zavisit ot nachal'noi funkcii mass zvezd, tempa zvezdoobrazovaniya v galaktike, modelei zvezdnoi evolyucii i drugih prichin. Potomu rezul'tat po Cas A ne mozhet byt' prinyat za srednee znachenie. Real'nost' slozhnee, i dlya ponimaniya processov formirovaniya pyli trebuyutsya dopolnitel'nye nablyudeniya. No to, chto nam uzhe izvestno, pozvolyaet utverzhdat', chto SNe II deistvitel'no yavlyayutsya effektivnym istochnikom pyli.

Vypusk 165. 01-13 avgusta 2007

arxiv:0708.0626 Sinhrotronnaya sverhobolochka v galaktike IC10: ostatok gipernovoi? (A synchrotron superbubble in the IC 10 Galaxy: a hypernova remnant?)
Authors: T.A. Lozinskaya, A.V. Moiseev
Comments: 4 pages, 3 EPS figures, Accepted to MNRAS (in Letters)

Vozmozhno, chto udalos' identificirovat' ostatok gipernovoi! Pokazano, chto sverhobolochka v galaktike IC10 veroyatnee vsego byla sformirovana za schet odnogo sil'nogo vzryva.


Vypusk 163. 01-19 iyulya 2007

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....


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 158. 12-21 maya 2007

arxiv:0705.2231 Zvezdnye mazery, okolozvezdnye obolochki i ostatki sverhnovyh (Stellar masers, circumstellar envelopes, and supernova remnants)
Authors: Athol J. Kemball
Comments: 16 pages, 2 figures, 2 tables: based on a review talk presented at IAU Symposium 242: Astrophysical masers and their environments, held at Alice Springs (Australia), March 12-16, 2007

Na moi vzglyad, tema zvezdnyh mazerov yavlyaetsya slegka "nedopopulyarizirovannoi". Pravda, dannyi obzor tut ne ochen' bol'shaya podmoga, ibo napisan on dlya teh, kto vsyu osnovu i tak uzhe znaet - t.e. dlya specialistov.


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.


Vypusk 149. 01-14 fevralya 2007

astro-ph/0702331 Statisticheskoe issledovanie nalakticheskih ostatkov sverhnovyh, ispol'zuya obzor PMN (A Statistical Study of Galactic SNRs using the PMN Survey)
Authors: M. Stupar et al.
Comments: 14 pages, 7 figures. Accepted for publishing in Astrophysics and Space Science

PMN - Parkes-MIT-NRAO. Eto radioobzor neba, kotoryi pozvolyaet izuchat' prakticheski vse ostatki sverhnovyh v nashei Galaktike. Tochnee, 164 iz 231 ostatka. Avtory vybrali 138 ostatkov, dlya kotoryh dannye imeyut dostatochno vysokoe kachestvo, i predstavili rezul'taty analiza etih ob'ektov. Vazhnym rezul'tatom raboty yavlyaetsya utochnenie parametrov metoda, kotoryi pozvolyaet opredelyat' rasstoyaniya do ostatkov.


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'.


Vypusk 133. 01-11 aprelya 2006

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 129. 20-28 fevralya 2006

astro-ph/0602552 Vozmozhnoe otkrytie novogo ostatka sverhnovoi v Cefee: obnaruzhenie edva vidimoi obolochki po rezul'tatam pervogo galakticheskogo obzora Spitcera (Tentative Discovery of a New Supernova Remnant in Cepheus: Unveiling an Elusive Shell in the Spitzer Galactic First Look Survey)
Authors: Patrick W. Morris et al.
Comments: 11 pages; accepted for publication in Astrophysical Journal Letters

Ochen' interesnaya rabota. Eshe do togo, kak ya nachal chitat' svezhii vypusk eprintov, moe vnimanie na etu rabotu obratil Dmitrii Vibe.

Po dannym obzora na kosmicheskom IK-teleskope im. Spitcera obnaruzhen chrezvychaino lyubopytnye ob'ekt. Priroda ego do konca neponyatna, no sushestvuet odna interesneishaya i dovol'no-taki veroyatnaya vozmozhnost': eto mozhet byt' ostatok sverhnovoi.

Teleskop im. Spitcera rabotaet na orbite otnositel'no nedavno. Eto chetvertaya (i poslednyaya) iz t.n. Velikih observatorii NASA (drugie proekty: Kosmicheskii teleskop , Komptonovskaya gamma-observatoriya i Chandra). Chtoby prodemonstrirovat' vozmozhnosti isntrumenta byl proveden bystryi "prosmotr" Galaktiki (Galactic First Look Survey). Imenno v ramkah etogo obzora i poluchen obsuzhdaemyi rezul'tat.

Nizhe pokazany tri izobrazheniya, poluchennye na Spitcere. Samoe nizhnee - eto izvestnyi ostatok sverhnovoi. Na srednem - novyi ob'ekt. Vidno, chto oni ochen' pohozhi. Odnako, na verhnem my ne vidim istochnika. Srednee i verhnee izobrazheniya otlichayutsya tem, chto polucheny na raznyh dlinah voln (na 24 i 8 mikronah). Eto dostatochno netipichno.


Oblast', v kotoroi obnaruzhen novyi ob'ekt, na dline volny 8 mikron. Sama obolochka na etih dlinah voln ne vidna.


Izobrazhenie otkrytogo ob'ekta na 24 mikronah.


Izobrazhenie izvestnogo ostatka sverhnovoi, poluchennoe na Spitcere (po dannym arhiva sputnika).

Po vsei vidimosti, eto v samom dele novyi interesnyi ostatok sverhnovoi. No, mozhet byt', eto planetarnaya tumannost'. Budem zhdat' novyh rezul'tatov po etomu istochniku.


Vypusk 125. 18-20 yanvarya 2006

astro-ph/0601451 Otkrytie 35 novyh ostatkov sverhnovyh v central'noi chasti Galaktiki (Discovery of 35 New Supernova Remnants in the Inner Galaxy)
Authors: C. L. Brogan, J. D. Gelfand, B. M. Gaensler, N. E. Kassim, T. J. Lazio
Comments: 5 pages; Accepted to ApJL

Po dannym obzora galakticheskoi ploskosti na VLA otkryto 35 novyh ostatkov sverhnovyh. Vse oni lezhat na galakticheskoi dolgote ot 4.5 do 22 gradusov, a po shirote v poyase +/-1.25 gradusov.



Vypusk 125. 18-20 yanvarya 2006

astro-ph/0601451 Otkrytie 35 novyh ostatkov sverhnovyh v central'noi chasti Galaktiki (Discovery of 35 New Supernova Remnants in the Inner Galaxy)
Authors: C. L. Brogan, J. D. Gelfand, B. M. Gaensler, N. E. Kassim, T. J. Lazio
Comments: 5 pages; Accepted to ApJL

Po dannym obzora galakticheskoi ploskosti na VLA otkryto 35 novyh ostatkov sverhnovyh. Vse oni lezhat na galakticheskoi dolgote ot 4.5 do 22 gradusov, a po shirote v poyase +/-1.25 gradusov.



Vypusk 119. 29 oktyabrya - 11 noyabrya 2005

obzor astro-ph/0511327 Shest' let nablyudenii ostatkov sverhnovyh na Chandre (Six Years of Chandra Observations of Supernova Remnants)
Authors: Martin C. Weisskopf, John P. Hughes
Comments: 82 pages, 28 figures, for the book Astrophysics Update 2

Veroyatno, mnogie pomnyat, chto "pervyi svet" Chandry - eto nablyudeniya ostatka sverhnovoi Cas A, prichem uzhe eti nablyudeniya priveli k otkrytiyu zagadochnogo tochechnogo ob'ekta v centre tumannosti, pro kotoryi do sih por ne yasno: neitronnaya zvezda eto ili chernaya dyra. V bol'shom materiale avtory summiruyut vsyu informaciyu po ostatkam sverhnovyh, poluchennuyu za 6 let na Chandre. Mnogo kartinok.


Vypusk 91. 01-14 noyabrya 2004

katalog astro-ph/0411083 Galakticheskie ostatki sverhnovyh: obnovlennyi katalog i statistika (Galactic Supernova Remnants: an Updated Catalogue and Some Statistics)
Authors: D. A. Green
Comments: 36 pages, 14 figures, including as an appendix a catalogue of 231 Galactic SNRs, to appear in the Bulletin of the Astronomical Society of India

Katalog Grina - samyi izvestnyi katalog ostatkov sverhnovyh. V stat'e predstavlena novaya versiya.

Katalog vklyuchaet 231 ostatok.

Vypusk 90. 25-31 oktyabrya 2004

Otkrytie !!! astro-ph/0410673 Komponent dvoinoi, porodivshei sverhnovuyu Tiho Brage 1572 goda (The binary progenitor of Tycho Brahe's 1572 supernova)
Authors: Pilar Ruiz-Lapuente et al.
Comments: 31 pages, 4 figures, accepted by Nature

Sverhnovaya Tiho Brage (SN 1572) odna iz dvuh istoricheskih sverhnovyh tipa Ia (vtoroi byla SN 1006) v nashei Galaktike. Sverhnovaya pervogo tipa proishodit, kak seichas schitaetsya, iz-za termoyadernogo vzryva belogo karlika, kotoryi dostig predel'noi (Chandrasekarovskoi) massy i poteryal ustoichivost'. Podobnyi process (uvelichenie massy belogo karlika) mozhet effektivno proishodit' tol'ko v dvoinoi sisteme: libo pri akkrecii veshestva s nevyrozhdennogo vtorogo kompan'ona, libo pri sliyanii dvuh belyh karlikov.

Pohozhe, chto v sverhnovoi Tiho realizovalsya imenno pervyi scenarii. Pri glubokom obzore central'noi chasti ostatka sverhnovoi byla naidena zvezda spektral'nogo klassa G0-G2 (podobnaya nashemu Solncu), kotoraya dvizhetsya so skorost'yu primerno v tri raza bol'shei, chem srednyaya skorost' zvezd v okrestnosti ostatka.

Sprava glubokii Habblovskii snimok. Sleva - shema dvizheniya zvezd na etom snimke. Kresty v centre shemy otmechayut geometricheskie centry rentgenovskogo izlucheniya Chandra (Ch), ROSAT (RO) i centr radioizlucheniya ostatka (Ra). Vokrug kazhdogo iz nih proveden krug radiusom 0.5" (sinie punktirnye linii). Sploshnoi krug - oblast', za predely kotoroi ni pri kakih usloviyah ne mogla vyletet' vtoraya komponenta predsverhnovoi.

Zvezda, otozhdestvlennaya so vtorichnym komponentom predsverhnovoi po sobstvennomu dvizheniyu, oboznachena bukvoi G. Esli eto otozhdestvlenie verno, to v 1572 godu sverhnovaya vzorvalas' v tochke, otmechennoi krestom i bukvami (Ty).

Krasnye tochki - polozheniya zvezd s vysokim sobstvennym dvizheniem na moment vzryva sverhnovoi.


Vypusk 89. 18-25 oktyabrya 2004

obzor astro-ph/0410464 Evolyuciya sverhnovyh v puzyryah vydutyh zvezdnym vetrom (The Evolution of Supernovae in Circumstellar Wind-Blown Bubbles I. Introduction and One-Dimensional Calculations)
Authors: Vikram V. Dwarkadas (University of Chicago)
Comments: 42 pages, 13 figures, subm. to ApJ

V obzore dostatochno podrobno rassmotrena sleduyushaya problema: massivnye zvezdy (>8-10Mo), vzryvayushiesya kak sverhnovye, obladayut ochen' sil'nym zvezdnym vetrom. Za vremya zhizni takoi zvezdy na glavnoi posledovatel'nosti i na bolee pozdnih evolyucionnyh stadiyah veter vyduvaet vokrug zvezdy kavernu razmerom do neskol'kih desyatkov parsek. Mezhzvezdnoe veshestvo, zapolnyavshee dannuyu oblast', okazyvaetsya sgrebennym v holodnyi, tonkii i ochen' plotnyi sloi. Sbroshennaya obolochka sverhnovoi, takim obrazom, vzaimodeistvuet ne s odnorodnoi sredoi, a s vydutoi vetrom kavernoi. Vazhneishim parametrom okazyvaetsya otnoshenie massy sgrebennogo vetrom veshestva k masse sbroshennoi obolochki sverhnovoi.

Opisannye rezul'taty byli polucheny dostatochno davno, no v dannom obzore oni dopolneny poslednimi detalyami i podrobno razobrany.


Vypusk 87. 01-10 oktyabrya 2004

astro-ph/0410081 Ostatok sverhnovoi Keplera: 400 let (Kepler's Supernova Remnant: The view at 400 Years)
Authors: W. P. Blair
Comments: 6 page

V oktyabre 2004 goda ispolnyaetsya 400 let vspyshke Sverhnovoi Keplera (SN 1604 - poslednyaya zafiksirovannaya Sverhnovaya v nashei Galaktike). Segodnya na ee meste nablyudaetsya rasshiryayushayasya tumannost' - ostatok sverhnovoi. Ih vseh istoricheskih sverhnovyh (a ih vsego neskol'ko) SN 1604 ostaetsya samoi zagadochnoi: do sih por sporyat o tipe etoi sverhnovoi, evolyucionnom sostoyanii porodivshei ee zvezdy (predsverhnovoi) i dazhe o rasstoyanii do ostatka (ono izvestno s tochnost'yu do dvoiki).


Vypusk 66. 19-26 yanvarya 2004

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.


(Arhiv Ostatki sverhnovyh:
v.2, 2003, v.1, 2002-2003)

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