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The R.A.P. Project (Reviews of Astro-Ph) 2003

Nasha Galaktika
(Arhiv Nasha Galaktika:
v.2, 2004, v.1, 2002-2003)

Vypusk 61. 16-30 noyabrya 2003

astro-ph/0311512 Pryamaya podpitka central'noi chernoi dyry Galaktiki zvezdnymi vetrami blizhaishih zvezd (Direct Feeding of the Black Hole at the Galactic Center with Radial Gas Streams from Close-In Stellar Winds)
Authors: Abraham Loeb (Harvard Univ.)
Comments: 4 pages, 2 figures, ApJL, submitted

Avtor pokazal, chto dlya ob'yasneniya ochen' nizkoi nablyudaemoi svetimosti central'noi chernoi dyry nashei Galaktiki (ob'ekta Sgr A*) dostatochno chasti zvezdnogo vetra ot massivnyh blizhaishih k chernoi dyre zvezd. Disk vokrug chernoi dyry ne obrazuetsya - zahvatyvaetsya tol'ko veshestvo dvizhusheesya pochti radial'no i zahvatyvaemoe chernoi dyroi.


Vypusk 59. 19-31 oktyabrya 2003

astro-ph/0310675 Kartirovanie dalekih uchastkov Mlechnogo Puti po BHB-zvezdam na 70 < r < 130 kpk (Mapping the Remote Milky Way Halo using BHB stars at 70 < r < 130 kpc)
Authors: L. Clewley et al.
Comments: 2 pages, 1 figure, to appear in the proceedings of the IAU Symposium 220: "Dark matter in galaxies", eds. S. Ryder, D.J. Pisano, M. Walker and K. Freeman, Sydney, July 2003, to be published in the ASP conference series

Vo mnogom vopros "gde granica nashei Galaktiki?" pohozh na vopros "gde granica Solnechnoi sistemy?". Na vtoroi mnogie otvechayut "za orbitoi Plutona", chto sovershenno neverno. Tochno takzhe klassicheskaya kartinka nashei Galaktiki, obryvayushayasya gde-to na 15-20 kpk ot centra ne sovsem verna. Pokuda est' zvezdy (pust' i nemnogchislennye) ili voobshe chto-to, chto vrashaetsya vokrug Mlechnogo Puti (t.e. gravitacionno s nim svyazano v, skazhem tak, podchinennom sostoyanii) i ne yavlyaetsya otdel'noi galaktikoi (tipa karlikovyh chlenov Mestnoi gruppy), to eto eshe nash Zvezdnyi Dom.

Samye dalekie zvezdy sostavlyayut t.n. galo galaktiki. I ih mozhno prosledit' na rasstoyaniya v 100-200 kpk. Avtory ispol'zovali dannye Sloanovskogo obzora (SDSS) po golubym zvezdam gorizontal'noi vetvi (BHB - blue horizontal branch). Blagodarya etim ob'ektam udalos' "propisat'" nashu Galaktiku do rasstoyanii v 130 kpk. Massa Mlechnogo Puti okazyvaetsya ravnoi 1.7(+3 -0.6) 1012 mass Solnca.

Rabota prodolzhaetsya. V budushem ozhidaetsya sushestvennoe snizhenie neopredelennosti v opredelenii massy.


astro-ph/0310788 Rezul'taty Archeops (Archeops results)
Authors: J.-Ch. Hamilton, A. Beno\^{\i}t and the Archeops Collaboration
Comments: 8 pages, 6 figures, to appear in C.R. Physique

Opisany rezul'taty poslednego poleta balonnogo eksperimenta Archeops po izmereniyu mikrovolnovogo izlucheniya. Krome, estestvenno, kosmologicheskih rezul'tatov, opisany i drugie. Osobyi interes predstavlyaet podrobnaya karta diffuznogo submillimetrovogo izlucheniya v ploskosti nashei Galaktiki (napomnim, chto pri postroenii polnoi karty reliktovogo fona prihoditsya vychitat' vklad Galaktiki, a eto sovsem neprostoe delo).


Karta Galaktiki na volne 353 GGc.


astro-ph/0310821 Vspyshki v blizhnem IK ot akkreciruemogo gaza vokrug sverhmassivnoi chernoi dyry v centre Galaktiki (Near-infrared flares from accreting gas around the supermassive black hole at the Galactic Centre)
Authors: R. Genzel et al.
Comments: 5 pages, 3 figures to appear in the Oct 30 issue of Nature

Chernaya dyra v centre nashei Galaktiki ochen' "tihaya". Ee aktivnost' yavlyaetsya chrezvychaino nizkoi vo vseh diapazonah spektra. Poetomu, lyuboe novoe obnaruzhennoe proyavlenie yavlyaetsya kraine vazhnym i interesnym.

Gruppa avtorov, kotorye uzhe horosho izvestny nashi chitatelyam po ih predydushim rabotam, posvyashennym centru Galaktiki, raportuet ob otkrytii vspyshek v blizhnem infrakrasnom diapazone. Vspyshki nablyudalis' v neposredstvennoi blizosti (neskol'ko millisekund dugi) ot chernoi dyry. U dvuh vspyshek byla otmechena periodichnost' s harakternym vremenem okolo 17 minut. Esli eto svyazano s vrasheniem gaza vokrug chernoi dyry, to my imeem delo s izlucheniem, voznikayushim v neposredstvennoi blizosti ot gorizonta. Krome togo, po etim dannym (esli interpretaciya verna) mozhno skazat', chto chernaya dyra ochen' bystro vrashaetsya.


Vypusk 56. 13-20 sentyabrya 2003

astro-ph/0309350 Prostranstvennoe raspredelenie oblastei HII v Galaktike (Spatial distribution of Galactic HII regions)
Authors: R. Paladini, G. DeZotti, R. D. Davies
Comments: 9 pages, 12 figures, 4 tables, accepted to MNRAS

V dannoi rabote priveden novyi detal'nyi analiz raspredeleniya oblastei HII (ionizovannogo vodoroda) v Galaktike. Dlya provedeniya dannogo issledovaniya byla ispol'zovana bolee polnaya baza dannyh, chem v predydushih rabotah, vklyuchayushaya v sebya 550 ob'ektov. Vnutri galakticheskoi orbity Solnca ("solnechnogo cikla") tolshina raspredeleniya HII okazalas' blizkoi k tolshine raspredeleniya OB-zvezd. Na bol'shih galaktocentricheskih rasstoyaniyah raspredelenie ob'ektov neskol'ko izognuto i ego tolshina uvelichivaetsya s udaleniem ot centra Galaktiki. Avtory takzhe podtverzhdayut obnaruzhennyi ranee gradient elektronnoi temperatury po radiusu Galaktiki.

Raspredelenie 550 oblastei HII v ploskosti Galaktiki.


Vypusk 55. 01-12 sentyabrya 2003

astro-ph/0309312 Prilivnye radiusy sharovyh skoplenii i massa Mlechnogo Puti (Tidal radii of globular clusters and the mass of the Milky Way)
Authors: Michele Bellazzini (INAF - Oss. Astron. di Bologna)
Comments: LaTex. 6 pages, 2 figures. Accepted for publication by MNRAS

Do sih por edinstvennym pryamym sposobom opredeleniya massy nashei Galaktiki bylo izmerenie skorostei krugovyh dvizhenii tel v ee udalennyh chastyah. Avtorom dannoi stat'i primenen drugoi sposob - cherez opredelenie prilivnyh radiusov (radiusov za kotorymi zvezdy "vyryvayutsya" iz skoplenii prilivnymi silami, deistvuyushimi so storony Mlechnogo Puti) dalekih (R>35 kpk) sharovyh skoplenii. Etot metod daet nezavisimuyu ocenku massy Galaktiki vnutri sfer s radiusami ot 35 do 100 kpk. Novyi rezul'tat horosho sovpadaet so starym (t.e. sootvetstvuet nablyudaemym na bol'shih rasstoyaniyah lineinym skorostyam krugovogo dvizheniya ravnym Vc=220+/-40 km/s. Naibolee tochnyi rezul'tat poluchen po sharovomu skopleniyu NGC 2419:

MGal(R<90 kpk) = 1.4(+2.9/-1.0)x1012 Mo.


Vypusk 51. 21-31 iyulya 2003

astro-ph/0307437 Konec ery MACHO: ogranicheniya na temnuyu materiyu po shirokim dvoinym Sistemam galo Galaktiki (The End of the MACHO Era: Limits on Halo Dark Matter from Stellar Halo Wide Binaries)
Authors: Jaiyul Yoo, Julio Chaname, Andrew Gould
Comments: submitted to ApJ, 6 pages including 7 figures
astro-ph/0307434 Shirokie dvoinye diska i galo iz Peresmotrennogo Lyutenovskogo Kataloga: zondy zvezdoobrazovaniya i MACHO (Disk and halo wide binaries from the Revised Luyten Catalog: probes of star formation and MACHO dark matter)
Authors: Shirokie dvoinye diska i galo iz Peresmotrennogo Lyutenovskogo Kataloga: zondy zvezdoobrazovaniya i MACHO (Disk and halo wide binaries from the Revised Luyten Catalog: probes of star formation and MACHO dark matter)
Comments: submitted to ApJ, 49 pages including 15 figures

Dve stat'i odnoi gruppy avtorov na blizkie temy.

MACHO (Massive Compact Halo Object) - massivnye kompaktnye ob'ekty galo Galaktiki. Proyavlyayut sebya v sobytiyah gravitacionnogo mikrolinzirovaniya, kogda proletayut mezhdu nami i dalekimi zvezdami ochen' blizko k luchu zreniya. Na chto eshe mogut vliyat' takie massivnye i mnogochislennye tela? Na shirokie dvoinye v galo Mlechnogo Puti: iz-za blizkih proletov MACHO samye shirokie pary budut razrushat'sya. Parametry granicy podobnogo razrusheniya shirokih dvoinyh zavisyat ot massy i chisla MACHO, kotorye ploho izvestny. Poskol'ku podobnyi zaval poka eshe ne nablyudaetsya v shirokih dvoinyh parah s uglovym rasstoyaniem mezhdu komponentami ot 5.5" do 900", to udaetsya dat' ogranicheniya na nekotorye parametry MACHO.

Vtoraya stat'ya (astro-ph/0307434) - eto analogichnaya, no gorazdo bolee podrobnaya i fundamental'naya rabota teh zhe avtorov, sdelannaya na osnove vyborki 1147 kandidatov v shirokie dvoinye sistemy ih Novogo Lyutenovskoko (Luyten) Kataloga. Zdes' vy naidete samye podrobnye raz'yasnenii, esli eta tema Vas zainteresuet.


Vypusk 50. 8-18 iyulya 2003

astro-ph/0307110 Nablyudeniya yarchaishei rentgenovskoi vspyshki ot SgrA* na XMM-Newton (XMM-Newton observation of the brightest X-ray flare detected so far from SgrA*)
Authors: D. Porquet et al.
Comments: Accepted for publication in A&A Letters. 4 pages, 2 figures, 1 tables

V centre nashei Galaktiki nahoditsya sverhmassivnaya chernaya dyra s massoi okolo 2-3 millionov mass Solnca. Kak izvestno, chernye dyry akkreciruyut okruzhayushee veshestvo, chto obychno privodit k poyavleniyu rentgenovskogo istochnika. Nashe galakticheskoe yadro v etom smysle yavlyaetsya ochen' neaktivnym: svetimost' chernoi dyry sostavlyaet poryadka odnoi desyatimillionnoi ot predel'noi svetimosti. Eto ochen' malo. Teoretikam prishlos' nemalo potrudit'sya, chtoby pridumat', kak mozhno ob'yasnit' takoe polozhenie del. Kak obychno teoretiki perestaralis': predlozheno neskol'ko mehanizmov, ob'yasnyayushih nizkuyu effektivnost' akkrecii. Kratko opishem dva mehanizma. Pervyi - advekciya. V etom sluchae goryachee veshestvo utekaet pod gorizont, ne uspev izluchit' zapasennuyu energiyu. Vtoroi - strui. Energiya unositsya ne elektromagnitnym izlucheniem, a perehodit v kineticheskuyu energiyu strui (ob etih mehanizmah my neodnokratno pisali - sm. arhiv nashih obzorov, temy "akkreciya" i "chernye dyry"). Vydelit' kakoi iz mehanizmov yavlyaetsya "edinstvenno pravil'nym" - ne udaetsya. Neobhodimo nablyudat'...

Nablyudeniya vyyavili interesnyi fenomen - rentgenovskie vspyshki. Vpervye eto bylo zaregistrirovano v 2000 g. na sputnike Chandra. V etoi stat'e avtory predstavlyayut dannye sputnika XMM-Newton po samoi yarkoi vspyshke. Svetimost' ee vse ravno nevelika: 3-4 1035 erg/s. Dlya ob'yasneniya vspyshek takzhe predlozheno neskol'ko mehanizmov. Chem bol'she nablyudenii - tem bol'she ogranichenii na teoreticheskie modeli. Novye nablyudeniya tut osobenno vazhny, t.k. zaregistrirovannaya vspyshka ne tol'ko samaya yarkaya, no ona eshe imeet ochen' myagkii spektr, simmetrichnuyu krivuyu bleska i ne pokazyvaet sushestvennyh spektral'nyh variacii so vremenem. Eto - novyi vyzov teoretikam.


astro-ph/0307258 Zvezdnyi potok v napravlenii anticentra Galaktiki (The Galactic Anticenter Stellar Stream)
Authors: Helio J. Rocha-Pinto et al.
Comments: 12 pages, 4 figures; submitted to the Astrophysical Journal Letters

Neskol'ko mesyacev nazad v sredstvah massovoi informacii aktivno obsuzhdalos' obnaruzhenie interesnoi struktury v nashei Galaktike: kol'cevoi struktury na rasstoyanii poryadka 17 kpk ot centra. V etoi rabote avtory provodyat tshatel'noe issledovanie etoi struktury i prihodyat k vyvodu, chto skoree vsego v napravlenii anticentra (sozvezdie Edinoroga) my vidim ostatok poglosheniya nebol'shoi galaktiki. T.e. po vsei vidimosti eto obrazovanie ne yavlyaetsya odnorodnoi strukturoi, okruzhayushei nashu Galaktiku.


astro-ph/0307291 Deistvitel'no holodnye zvezdy i istoriya zvezdoobrazovaniya v centre Galaktiki (Really Cool Stars and the Star Formation History at the Galactic Center)
Authors: R. D. Blum et al.
Comments: ApJ, accepted. Latex, 65 pages including 19 figures

Bol'shaya stat'ya, posvyashennaya istorii zvezdoobrazovaniya v oblasti galakticheskogo centra.

S odnoi storony izvestno, chto v centre Galaktiki mnogo molodyh zvezd, t.e. nedavno tam byla dovol'no moshnaya vspyshka zvezdoobrazovaniya. S drugoi storony yasno, chto tam mnogo ochen' staryh zvezd. Ispol'zuya ochen' bol'shuyu vyborku ob'ektov, avtory pytayutsya detal'no vosstanovit' istoriyu zvezdoobrazovaniya v etom neprstom raione nashego zvezdnogo ostrova. Osnovnye vyvody takovy: bolee 75 procentov zvezd vnutri neskol'kih parsek imeyut vozrast bolee 5 milliardov let, temp zvezdoobrazovaniya sushestvenno izmenyalsya so vremenem.



Vypusk 46. 1-15 iyunya 2003

astro-ph/0306074 Nuzhna eshe odna chernaya dyra v centre Galaktiki (The need for a second black hole at the Galactic center)
Authors: Brad Hansen, Milos Milosavljevic
Comments: 5 pages, 2 postscript figures, submitted to ApJ letters The introduction section has been updated since submission to ApJ

Pohozhe vse uzhe soglasilis' s nalichiem chernoi dyry massoi primerno 3.106 Mo v centre nashei Galaktiki. Eto utverzhdenie podtverzhdaetsya kak infrakrasnymi nablyudeniyami istochnika Sagitarrius A*, tak i dinamikoi zvezd vnutri central'nogo 0.1 pk.

Voprosy vyzyvaet drugoi fakt - naibolee yarkie zvezdy na rasstoyanii 0.1 pk, sobstvennye dvizheniya kotoryh nablyudayutsya, yavlyayutsya massivnymi i, sledovatel'no, molodymi. Otkuda oni vzyalis'? Tam gde oni nahodyatsya seichas im obrazovat'sya prosto ne iz chego. Priblizit'sya k central'noi chernoi dyre s bOl'shih rasstoyanii (naprimer s 1 pk) pod deistviem dinamicheskogo treniya oni by ne smogli - harakternoe vremya podobnoi diffuzii sushestvenno prevyshaet vremya zhizni massivnyh zvezd.

Avtory dannoi raboty predpolagayut, chto nablyudaemye nami zvezdy byli sbrosheny so svoih orbit za predelami 1 pk chernoi dyroi promezhutochnoi massy (103-104 Mo), obrashayusheisya vokrug centra Galaktiki po dostatochno udalennoi orbite. Podtverzhdeniem sushestvovaniya vtoroi chernoi dyry mozhet posluzhit' obnaruzhenie smesheniya svyazannogo s central'noi chernoi dyroi radioistochnika pod deistviem gravitacii vtoroi dyry. Nesmotrya na to, chto massa vtoroi dyry sostavlyaet dolyu procenta ot central'noi - sovremennaya astrometriya mozhet zaregistrirovat' podobnoe smeshenie.


Vypusk 42. 1-9 maya 2003


astro-ph/0305074 Otkrytie Sgr A* (The Discovery of Sgr A*)
Authors: W.M.Goss, Robert L.Brown, K.Y.Lo
Comments: 8 pages,2 figures. Conference proceedings: "The central 300 parsecs of the Milky Way", editors A.Cotera, H.Falcke, T.R.Geballe, S.Markoff

Nebol'shoi rasskaz o rannih (60-e - 80-e gg.) nablyudeniyah centra Galaktiki v radiodiapazone. Istochnik Sgr A* - eto sobstvenno nasha sverhmassivnaya chernaya dyra. Tochnee skazat' tak oboznachili (v 1982 g.) radioistochnik v samom centre Galaktik, vnutri kotorogo sidit nasha chernaya dyra.


Vypusk 40. 20-25 aprelya 2003

astro-ph/0304383 ISOGAL: glubokii obzor vnutrennih chastei Mlechnogo Puti na ISO na 7 i 15 mikronah i s pomosh'yu DENIS v blizhnem IK (ISOGAL: A deep survey of the obscured inner Milky Way with ISO at 7 and 15 micron and with DENIS in the near-infrared)
Authors: A. Omont et al.
Comments: A&A in press. 19 pages,10 Postscript figures

ISO - Infrared Space Observatory. ISOGAL - obzor central'noi (zakrytoi pyl'yu) chasti Galaktiki na etoi observatorii. Na 16 kvadratnyh gradusah, pripodnyav pylevuyu zavesu, uchenye uvideli okolo 100 000 istochnikov. V osnovnom eto zvezdy: kak molodye, tak i uzhe proevolyucionirovavshie (zvezdy asimptoticheskoi vetvi, krasnye giganty). K stat'e prilagayutsya dovol'no interesnye kartinki.


astro-ph/0304351 Raspredelenie izlucheniya galakticheskogo baldzha na |b|>2o po RXTE skanam galakticheskogo centra (Distribution of the Galactic Bulge emission at |b|>2deg according to th RXTE Galactic Center scans)
Authors: M.Revnivtsev
Commnets: 6 pages, 7 figures. Submitted to Astronomy & Astrophysics

Astronomam inogda udaetsya poluchit' ochen' neobychnye kartinki.

Rentgenovskii sputnik RXTE (Rossi X-Ray Timing Explorer) issledoval nebo samymi raznymi sposobami. Odin iz nih - rentgenovskie skany - kogda nablyudalis' vse ob'ekty v ochen' uzkoi, no dlinnoi poloske. Bol'shinstvo takih skanov provodilos' vblizi centra nashei Galaktiki, i ih nabralos' tak mnogo, chto stalo vozmozhnym postroit' kartinu centra tol'ko po etim dannym. Poluchennaya "karta" pokazana na pervom risunke (chernota skanov proporcional'na zaregistrirovannomu potoku izlucheniya, kruzhkami obvedeny izvestnye rentgenovskie istochniki). Na vtorom risunke - poluchennyi po etim zhe dannym "razrez" Galaktiki (chernye simvoly - rentgenovskaya svetimost' krasnaya krivaya - intensivnost' izlucheniya v linii CO, sinyaya gistogramma - kolichestvo ostatkov sverhnovyh na bin).


astro-ph/0304361 Kinematika prilivnogo razrusheniya galaktiki-praroditelya Omega Centavra (Kinematics of Tidal Debris from Omega Centauri's Progenitor Galaxy)
Authors: Arihiro Mizutani et al.
Commnets: 14 pages, 3 figures

Omega Centavra - odno iz samyh bol'shih i massivnyh sharovyh skoplenii nashei Galaktiki. Nekotorye iz scenariev ego proishozhdeniya predpolagayut, chto kogda-to ono bylo yadrom karlikovoi galaktiki - sputnika Mlechnogo Puti. No eta galaktika nahodilas' slishkom bystro i byla razrushena prilivnymi silami, sohranilos' - v vide sharovogo skopleniya - tol'ko yadro, ee naibolee plotnaya i kompaktnaya chast'. Ostal'nye zvezdy byli razbrosany po Galaktike. Kakimi kinematicheskimi svoistvami oni teper' obladayut? Eti zvezdy popadayut v sfericheskuyu sostavlyayushuyu Galaktiki, oni imeyut vysokie (~300 km/s) radial'nye skorosti. Sushestvennaya chast' etih zvezd imeet obratnoe dvizhenie. Rezul'taty provedennyh avtorami raschetov pokazany na risunke.



Vypusk 38. 01-11 aprelya 2003

V svyazi s novymi dannymi nablyudenii uchenyh vse bol'she volnuet vopros "Chto proishodit v centre Galaktiki?" Za proshedshie dni krome bol'shogo chisla rabot po sverhmassivnym chernym dyram v drugih galaktikah poyavilas' seriya ochen' raznyh statei, posvyashennyh central'noi oblasti nashego Mlechnogo Puti. Takzhe rasskazhem o rabotah v poryadke ih poyavleniya v Arhive.

Nachnem s teoreticheskoi raboty MakMillana i Zvarta "Sud'ba zvezdnogo skopleniya vblizi centra Galaktiki: analiticheskie rassuzhdeniya" (astro-ph/0304022). V dannoi rabote izuchaetsya sud'ba molodogo zvezdnogo skopleniya, padayushego na galakticheskii centr s otnositel'no nebol'shogo rasstoyaniya (neskol'ko desyatkov parsek).
Poskol'ku avtory reshili rassmotret' problemu analiticheski, im konechno zhe prihoditsya delat' uproshayushie predpolozheniya. Odnako, eto lish' stat'ya N1. A Portegies Zwart izvesten i kak ochen' horoshii specialist po komp'yuternomu modelirovaniyu....

Perehodim k drugim rabotam.

Sgr A* - "nasha" sverhmassivnaya chernaya dyra. Tochnee, eto oboznachenie istochnika v centre nashei Galaktiki, kotoryi neposredstvenno svyazan s chernoi dyroi.

Poslednie 10 let gruppa nemeckih uchenyh poluchaet vse bolee i bolee tochnye dannye po dvizheniyu zvezd vokrug centra Galaktiki. Stat'ya "Polozhenie, dvizhenie i massa Sgr A*" - eto ih ocherednoi "otchet o prodelannoi rabote".

Otnositel'no nedavno oni nachali ispol'zovat' novuyu apparaturu, rabotayushuyu v infrakrasnom diapazone, chto pozvolilo sushestvenno povysit' tochnost' nablyudenii. V dannoi rabote oni dayut nizhnii predel na massu chernoi dyry 4 105 solnechnyh mass. Voobshe seichas nailuchshie ocenki massy dayut poryadka 2 106 mass Solnca. No, uchityvaya specifichnost' astronomii, tochnyi nizhnii predel konechno zhe ne budet lishnim... (Sm. takzhe stat'yu etoi gruppy o central'nom zvezdnom skoplenii nashei Galaktiki - astro-ph/0304197).

Kratko rasskazhem eshe o neskol'kih stat'yah.

Centr Galaktiki seichas ochen' aktivno issleduetsya kak eksperimentatorami, tak i teoretikami. Sm., naprimer, stat'yu Quataert "Radiatively Inefficient Accretion Flow Models of Sgr A*" (astro-ph/0304099), posvyashennuyu vazhnomu voprosu o nizkoi effektivnosti akkrecii na nashu sverhmassivnuyu chernuyu dyru (tut zhe i drugaya stat'ya Quataert v soavtorstve s Feng Yuan, gde avtory takzhe izuchayut vopros o nizkoi effektivnosti akkrecii). V sleduyushei teoreticheskoi stat'e "X-ray flares from Sgr A*: star-disk interactions?" (astro-ph/0304126) razbiraetsya problema rentgenovskih vspyshek ot Sgr A*. Ne otstayut i eksperimentatory: Lu, Wang, Lang "The Chandra Detection of Galactic Center X-ray Features G359.89-0.08 and G359.54+0.18" (astro-ph/0304101). Zdes' opisyvaetsya otkrytie dvuh lyubopytnyh rentgenovskih istochnikov v neposredstvennoi blizi ot SgrA*.


(Arhiv Nasha Galaktika:
v.2, 2004, v.1, 2002-2003)

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