The R.A.P. Project (Reviews of Astro-Ph)
Akkreciya
Authors: G.S. Bisnovatyi-Kogan, R.V.E. Lovelace
Comments: 143 pages, 25 figures New Astronomy Reviews 45 (2001) 663-742
V stat'e daetsya podrobnyi obzor advekcionno-dominirovannyh diskov, a takzhe obsuzhdaetsya rol' magnitnyh polei v diskovoi akkrecii.
Rabota napisana okolo 2 let nazad. Nekotoruyu novuyu diskussiyu mozhno naiti v svezhei korotkoi zametke Novaka (astro-ph/0207624).
Authors: Igor V. Igumenshchev
Comments: 10 pages, will appear in ApJL
Hotya pervye raboty po teorii akkrecii poyavilis' eshe do Vtoroi Mirovoi Voiny, tam ostaetsya eshe ochen' mnogo neyasnogo. Sovremennaya teoriya diskovoi akkrecii byla sozdana 30 let nazad [ Shakura 1972, Shakura, Syunyaev 1973] (voobshe-to eto byl by horoshii povod dlya krupnoi konferencii, no ...). Odnako, v poslednie gody nachali obsuzhdat'sya rasshireniya standartnogo scenariya: t.n. advekcionno-dominirovannye i konvekcionno-dominirovannye techeniya. Voprosu o perenose ugolovogo momenta v techeniyah poslednego tipa i posvyashena stat'ya.
Authors: A. Merloni
Comments: 10 pages, 1 colour figure. Latex macro sprocl.sty. Invited review, to be published in the proceedings of the 5th Italian AGN Meeting "Inflows, Outflows and Reprocessing around black holes" (2002)
Daetsya obzor po akkrecii na chernye dyry. V korotkoi zametke prakticheski bez formul dayutsya vse osnovnye idei. Odnako, po toi zhe prichine dlya specialistov stat'ya malo interesna. Ochen' polezna dlya studentov-aspirantov, i, kak govoritsya, dlya "specialisto smezhnyh special'nostei".
Authors: Jose A. Font, Frederic Daigne
Comments: 12 pages, 3 figures, accepted for publication in ApJL
Issleduetsya ustoichivost' diskov dlya parametrov, primenyaemyh pri modelirovanii kosmicheskih gamma-vspleskov. T.e. eto ne tesnaya dvoinaya sistema, a bystrovrashayushayasya chernaya dyra s tolstym torom vokrug. Uchteny effekty OTO. Avtory nahodyat neustoichivost' na dinamicheskom masshtabe vremeni.
(po angliiski Ultra-Luminous ili Super--Luminous, inogda bez tire) Yarkie rentgenovskie istochniki mogut voznikat' po raznym prichinam. Odin iz klassov takih ob'ektov - eto tesnye dvoinye sistemy, sostoyashie iz kompaktnogo ob'ekta (neitronnoi zvezdy ili chernoi dyry) i normal'noi zvezdy. Veshestvo s normal'nogo komponenta popadaet v pole tyagoteniya kompaktnogo (pri zapolnenii polosti Rosha ili cherez zvezdnyi veter) i, v konce koncov, padaet na ego poverhnost'. Pri etom izluchaetsya bol'shoe kolichestvo energii (gravitacionnoi) v vide zhestkogo rentgenovskogo izlucheniya. Odnako, esli temp akkrecii slishkom velik, to davlenie izlucheniya okazyvaetsya bol'she, chem silya tyagoteniya, i vse veshestvo uzhe ne mozhet upast' na poverhnost' kompaktnogo ob'ekta. Odnovremenno spektr izlucheniya smeshaetsya v myagkuyu oblast', tak kak rentgen pogloshaetsya i pererabatyvaetsya v okruzhayushei kompaktnyi ob'ekt obolochke. Predel'naya svetimost' nazyvaetsya Eddingtonovskoi, ona proporcional'na masse kompaktnogo ob'ekta i dlya 1 Mo ravna 1.3.1038 erg/s. Esli zhe my vidim rentgenovskii istochnik so svetimost'yu poryadka LX=1039-1041 erg/s, to sleduet dumat', chto v etom istochnike nahoditsya sushestvenno bolee massivnyi ob'ekt, chem standartnaya neitronnaya zvezda (s tipichnoi massoi 1.4 Mo). Okonchatel'noi yasnosti s prirodoi sverhizluchayushih istochnikov net, v nashei Galaktike takie ob'ekty neizvestny, no v sosednih oni nablyudayutsya.
Authors: J.M.Miller, G.Fabbiano, M.C.Miller et al.
Commets: 5 pages, 3 color figures, uses emulateapj.sty and apjfonts.sty, ApJL subm
Eta stat'ya osnovana na analize rentgenovskih nablyudenii blizkoi spiral'noi galaktiki NGC 1313 co sputnika XMM-Newton. V etoi galaktike nablyudayutsya dva sverhizluchayushih rentgenovskih istochnika so svetimostyami (pri izotropnom izluchenii) LX = 2.0.1040 erg/s i LX = 6.6.1039 erg/s dlya istochnikov NGC 1313 X-1 i X-2 v diapazone 0.2-10 keV, sootvetstvenno (dlya rascheta svetimosti rasstoyanie do galaktiki schitalos' ravnym 3.7 Mpk). Spektr izlucheniya etih istochnikov sushestvenno bolee myagkii (kT=150 eV), chem u drugih kandidatov v chernye dyry (gde tipichnaya temperatura kT=1 keV). Tak kak izluchenie v takih ob'ektah idet ot akkrecionnogo diska, to polagaya, chto ego vnutrennii krai blizok k poslednei ustoichivoi orbite (t.e. nahoditsya na rasstoyanii 3Rg ot centra chernoi dyry), my poluchaem spektroskopicheskuyu ocenku massy ob'ekta: MBH=100Mo. V etom sluchae ukazannye vyshe znacheniya svetimostei okazyvayutsya blizki k Eddingtonovskim, chto sluzhit eshe odnim podtverzhdeniem takoi ocenki massy.
Authors: Ji-Feng Liu et al
Commets: accepted for ApJ Letter
Chto takoe sverhizluchayushie istochniki - do konca ne yasno (pervoe, chto nado ponyat': izotropno izluchenie ili zhe kollimirovano) . Poetomu lyubaya novaya informaciya o nih predstavlyaet interes. Tak v sverhizluchayushem istochnike ULX M51 X-7 v galaktike M51, rentgenovskaya svetimost' kotorogo menyaetsya v predelah LX=1039-1041 erg/s, po nablyudeniyam c Chandra byl naiden period 2.1 chasa. Avtory predpolagayut, chto etot ob'ekt yavlyaetsya malomassivnoi dvoinoi sistemoi, sostoyashei iz normal'noi zvezdy massoi 0.2-0.3 Mo i kompaktnogo ob'ekta (neitronnoi zvezdy ili chernoi dyry), a 2.1 chasa - ee orbital'nyi period.
Authors: Ji-Feng Liu et al Journal-ref: 2002ApJ...580L..31L
Eshe odin sverhizluchayushii istochnik, ULX NGC 3031 X-11, v galaktike M81 otozhdestvlen v optike (o vazhnosti podobnoi informacii smotri zdes'). Svetimost' etogo istochnika v rentgene sostavlyaet LX~2.1039 erg/s, a v optike na ego meste my vidim massivnuyu moloduyu zvezdu klassa O8V. Vtorym komponentom etoi sistemy, po-vidimomu, yavlyaetsya chernaya dyra s massoi priblizitel'no ravnoi 18 Mo.
Authors: V.S. Beskin, A.D. Tchekhovskoy
Commets: 9 pages, 1 figure, uses sc3conf.sty, to appear in Proc. Third Sakharov Conference on Physics, A.Semikhatov et al. (eds.), Scientific World, Moscow (2003)
Otechestvennaya rabota - iz FIANa (doklad na etu temu budet sdelan v konce dekabrya v Moskve na konferencii HEA-2002). Horosho izvestnyi fakt, chto na rasstoyanii 3Rg ot Shvarcshil'dovskoi chernoi dyry dvizhenie probnoi chasticy po krugovoi orbite stanovitsya neustoichivym i ona padaet na chernuyu dyru. S chasticami v akkrecionnom diske, vnutrennii krai kotorogo dohodit do poslednei ustoichivoi orbity, proishodit tozhe samoe - oni padayut vnutr'. No kak pri etom vedet sebya vertikal'naya struktura diska vnutri etoi granicy? Otvet, poluchennyi avtorami pokazan na risunke. Granica ustoichivogo diska raspolozhena sleva, chernaya dyra - sprava.
Authors: O.M.Blaes
Commets: in "Accretion Disks, Jets, and High Energy Phenomena in Astrophysics", Proceedings of Session LXXVIII of Les Houches Summer School, Chamonix, France, August 2002, F.Menard, G. Pelletier, G.Henri, V. Beskin, and J. Dalibard eds. (EDP Science: Paris and Springer: Berlin), in preparation
Omer Blaes - ochen' izvestnyi astrofizik, a, mozhet byt', uzhe i klassik nauki. Ego nebol'shoi kurs lekcii posvyashen teorii akkrecionnyh diskov s osobym uporom na processy proishodyashie v yarkih rentgenovskih istochnikah, soderzhashih chernye dyry. V kurse rassmotreny: standartnaya model' Shakury-Syunyaeva, formirovanie spektrov izlucheniya, perenos uglovogo momenta v diske, rol' irradiacii (oblucheniya diska central'nym istochnikom) i magnitogidrodinamicheskih processov. Slozhnyh formul kurs ne soderzhit.
Authors: Christopher S.Reynolds, Michael A.Nowak
Commets: 103 pages, 21 figures. Review article, accepted for publication in Physics Reports
Fakticheski eto kniga.Avtory podrobneishim obrazom razbirayut, kak po nablyudeniyam fluorescentnyh linii mozhno provodit' detal'nuyu diagnostiku akkreciruyushih chernyh dyr v tesnyh dvoinyh sistemah i v yadrah galaktik.
Authors: Keith Horne
Commets: To appear in: Astronomical Telescopes and Instrumentation, Future EUV, UV, and Visible Space Astrophysics Missions and Instrumentation, 22-28 Aug 2002, Waikoloa, HI, SPIE Proc 4856
Keit Horn (Keith Horne) yavlyaetsya izvestnym specialistom po tomografii akkrecionnyh diskov. Takoi vid issledovaniya vozmozhen, naprimer, v zatmennyh dvoinyh sistemah. V etoi stat'e rech' idet ob issledovanie akkrecionnyh potokov v aktivnyh yadrah galaktik, gde vtorogo ob'ekta net! Zdes' tehnologiya sovsem drugaya. Issleduetsya "eho" - pereizluchennyi svet. Izmeryayutsya vremennye zaderzhki, doplerovskii sdvig i t.d. Poka metodika nahoditsya v stadii stanovleniya. Avtor nadeetsya, chto v skorom budushem ona pomozhet uznat' mnogo novogo o processah v aktivnyh yadrah galaktik.
Authors: Andrew I. MacFadyen
Commets: 7 pages, to appear in Proc. "From Twilight to Highlight - The Physics of Supernovae" ESO/MPA/MPE Workshop, Garching July 2002
V rabote rassmatrivaetsya svyaz' mezhdu vzryvami sverhnovyh, vrasheniem massivnyh zvezd (sm. takzhe vyshe) i gamma-vspleskami. V modeli kollapsara v nachale iz yadra massivnoi zvezdy obrazuetsya chernaya dyra, na kotoruyu idet moshnaya akkreciya iz ochen' plotnogo akkrecionnogo diska. Po mneniya avtora raboty nalichie takih diskov i razliyanyi uglovoi moment u raznyh zvezd-praroditelei mogut ob'yasnit' nekotorye pekulyarnye tipy sverhnovyh, a takzhe gamma-vspleski, nesoprovozhdayushiesya obychnoi sverhnovoi.
Authors: A. A. Shatskiy
Commets: 7 pages, 1 figures
Rasschitana struktura i amplituda elektromagnitnyh polei porozhdaemyh vrashayushimsya vokrug chernoi dyry diskom s vmorozhennym v nego magnitnym polem. Vokrug diska - vakuum.
Authors: D. Proga, M.C. Begelman
Commets: 30 pages, submitted in ApJ
Opisyvaetsya modelirovaniya akkrecii na chernuyu dyru, v sluchae kogda padayushee veshestvo obladaet nebol'shim uglovym momentom. Pokazano, chto nalichie momenta privodit k sushestvennomu umen'sheniyu tempa akkrecii po sravneniyu s formuloi Bondi (ot sebya dobavim, chto eto mozhet byt' vazhno pri raschete akkrecii na odinochnye chernye dyry, t.k. akkreciruyushaya mezhzvezdnaya sreda turbulizovana).
Author: Banibrata Mukhopadhyay
Commets: 36 pages including 12 figures; aaspp4 style; To appear as an invit article in a collected volume "Progress in Astrophysics", Nova Science Publishers, Inc.; The resolution of Figs. 1-6 is made very poor (to fit all those in 4Mb limit of archive), contact the Author if you want the figures with perfect resolution
Reshat' zadachi akkrecii neposredstvenno v ramkah OTO dostatochno tyazhelo. Poetomu vmesto iskrivlennogo prostranstva mozhno popytat'sya vvesti psevdo-N'yutonovskii potencial v kotorom dvizhenie chastic opisyvaetsya pravil'no. Eto udaetsya sdelat' nevrashayushihsya neitronnyh zvezd i chernyh dyr. Dlya vrashayushihsya ob'ektov oboitis' odnim potencialom ne udaetsya. Avtor podrobno rassmatrivaet kak edinym obrazom mozhno vvesti takie potencialy i v kakih sluchayah dannyh podhod rabotaet.
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: Ramesh Narayan, Jeremy S. Heyl
Commets: 56 pages, 19 figures, submitted to the Astrophysical Journal
Bol'shaya original'naya teoreticheskaya rabota, zhestko privyazannaya k real'nym nablyudatel'nym dannym. Rassmatrivaetsya "sud'ba" veshestva (vodoroda i geliya), nakopivshegosya na poverhnosti neitronnoi zvezdy v processe akkrecii. Delo v tom, chto v takom veshestve mogut nachinat'sya termoyadernye reakcii. Pri etom nablyudaetsya rentgenovskaya vspyshka (istochniki takoi aktivnosti nazyvayutsya "rentgenovskie barstery").
Publikacii s klyuchevymi slovami:
astrofizika - obzory - ekzoplaneta - Planety u drugih zvezd
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