The R.A.P. Project (Reviews of Astro-Ph)
Sverhnovye
Authors: Shizuka Akiyama, J. Craig Wheeler et al.
Comments: 42 pages, including 15 figures. Accepted for publication in ApJ
Poka nikto ne znaet kak vzryvayutsya sverhnovye. Est' tri osnovnyh mehanizma (zdes' privoditsya otryvok iz nashego obzora):
Pervyi mehanizm ob'edinyaet klassicheskuyu model' "otskoka" ("bounce") padayushih vneshnih sloev yadra predsverhnovoi ot sformirovavshegosya i stavshego zhestkim sverhplotnogo ostatka sverhnovoi (goryachei proto-NZ) s neitrinnymi mehanizmami, v kotoryh obrazovavshayasya v rezul'tate otskoka udarnaya volna v dal'neishem podpityvaetsya neitrinnym izlucheniem goryachego yadra. Eto samaya pervaya i dolgoe vremya schitavshayasya osnovnoi model' vzryva sverhnovoi. Hotya ranee v ramkah etoi modeli neskol'ko raz udavalos' ob'yasnit' vspyshku sverhnovoi, posleduyushie bolee tochnye issledovaniya otvergali eti naidennye vozmozhnosti. Na segodnya dannyi mehanizm ne ob'yasnyaet sbros obolochki sverhnovoi ni v sfericheski simmetrichnom, ni v osesimmetrichnom (s vrasheniem) sluchayah. Est' nadezhda, chto situaciyu mogla by ispravit' krupnomasshtabnaya neitrinnaya konvekciya. V nastoyashee vremya v dannom napravlenii vedutsya intensivnye issledovaniya.
Drugoi mehanizm (Imshennik 1992) svyazan s deleniem bystrovrashayushegosya kollapsiruyushego yadra zvezdy na 2 chasti, po krainei mere odna iz kotoryh dolzhna byt' neitronnoi zvezdoi. Zatem chasti dvoinogo yadra sblizhayutsya iz-za gravitacionnogo izlucheniya, poka men'shaya po masse (i bol'shaya po razmeru) komponenta ne zapolnit svoyu polost' Rosha. Sblizhenie dvoinogo yadra mozhet dlit'sya ot neskol'kih minut do neskol'kih chasov. Posle etogo nachinaetsya peretekanie veshestva do teh por, poka massa men'shei komponenty ne dostignet nizhnego predela mass NZ (okolo 0.09M), pri kotorom proishodit vzryvnaya deneitronizaciya malomassivnoi neitronnoi zvezdy. Takoe dopolnitel'noe vydelenie energii, proishodyashee dostatochno daleko ot centra kollapsiruyushei zvezdy, mozhet effektivno sbrosit' ee obolochku. Etot mehanizm mozhet deistvovat' tol'ko u naibolee bystro vrashayushihsya predsverhnovyh. Problema dannogo scenariya zaklyuchena v tom, chto poka eshe nikomu ne udalos' vosproizvesti delenie yadra predsverhnovoi pri kollapse.
Poslednii iz rassmatrivaemyh nami mehanizmov vzryvov sverhnovyh - magnitorotacionnyi - byl predlozhen G.S.Bisnovatym-Koganom v 1970 g. Ideya etogo mehanizma ochen' prosta - sbros obolochki proizvoditsya magnitnym polem bystro vrashayusheisya NZ. Pri etom obolochka uskoryaetsya za schet tormozheniya vrasheniya neitronnoi zvezdy. Poskol'ku na samom dele eta prostaya ideya ob'edinyaet v sebe generaciyu i usilenie magnitnyh polei i slozhnuyu trehmernuyu gidrodinamiku s sil'nym vliyaniem perenosa izlucheniya, to realistichnye raschety dannogo scenariya kraine zatrudneny. Rezul'taty dvumernyh raschetov pokazyvayut, chto magnitorotacionnyi mehanizm mozhet peredat' neskol'ko procentov vrashatel'noi energii kompaktnogo ostatka v kineticheskuyu energiyu obolochki. Kak pokazyvayut upomyanutye raschety, magnitorotacionnyi vzryv (stadiya na kotoroi proishodit sushestvennoe uskorenie i sbros obolochki) dlitsya 0.01-0.1 s. Odnako emu predshestvuet faza "nakrutki", na kotoroi toroidal'noe magnitnoe pole lineino usilivaetsya do kriticheskoi velichiny pri kotoroi proishodit sbros obolochki. Dlitel'nost' etoi s zavisit ot velichiny nachal'nogo magnitnogo polya NZ i ot skorosti ee vrasheniya i mozhet menyat'sya ot dolei sekundy do minut (i dazhe chasov). Dlya dannogo mehanizma trebuetsya dostatochno bystroe vrashenie NZ (period poryadka neskol'kih millisekund), odnako ne stol' bystroe, kak v mehanizme s deleniem yadra.
V rassmatrivamoi stat'e Akiyamy i dr. issleduetsya magnitovrashatel'naya neustoichivost', privodyashaya k rostu magnitnogo polya pri kollapse. Bipolyarnye potoki, voznikayushie blagodarya neustoichivosti, mogut sushestvenno vliyat' na vzryv, ili dazhe yavlyat'sya ego osnovnym "dvigatelem".
Authors: Ken'ichi Nomoto, Keiichi Maeda, Hideyuki Umeda, Takuya Ohkubo, Jingsong Deng, Paolo Mazzali
Comments: Invited talk at IAU Symposium 212, "A Massive Star Odyssey, from Main Sequence to Supernova", to be published in the Proceedings (San Francisco: ASP) eds. K.A. van der Hucht, A. Herrero, & C. Esteban, 9 pages
Daetsya obzor po nukleosintezu v gipernovyh. Oni ochen' populyarny v poslednee vremya v svyazi s nekotorymi modelyami gamma-vspleskov. Odnako, poka net odnoznachnyh vyvodov v pol'zu samogo sushestvovaniya gipernovyh. Issledovaniya v oblasti nukleosinteza mogut pomoch' v reshenii voprosa o real'nosti takih supervzryvov.
Authors: Mario Hamuy
Comments: 25 pages, 7 figures, accepted for Part 1 of Astrophysical Journal
Avtor analiziruet fotometricheskie i spektroskopicheskie dannye o 24 sverhnovyh vtorogo tipa. Opredelyayutsya takie parametry kak energetika vzryva, massy i radiusy predsverhnovyh. Poluchaetsya, chto bolee massivnye predsverhnovye dayut bolee moshnye vzryvy. Bolee moshnye sverhnovye dayut bol'she nikelya. Pohozhie sootnosheniya est' dlya sverhnovyh tipov Ib/c, chto mozhet govorit' o tom, chto fizika tam pohozhaya.
Authors: Carles Badenes, Eduardo Bravo
Comments: 4 pages, 3 figures. Proceedings of the ESO/MPA/MPE Workshop 'From Twilight to Highlight', the Physics of Supernovae. Garching July 29 - 31, 2002
Konkretnye mehanizmu vspyshek sverhnovyh raznyh tipov ostayutsya neizvestnymi. Avtory pytayutsya vytashit' kakuyu-to informaciyu ob etom iz nablyudayushihsya ostatkov sverhnovyh. Oni rassmatrivayut spyshki tipa Ia. Stroitsya gidrodinamicheskaya model' vzaimodeistviya vybrosa s okruzhayushei sredoi. Avtory pytayutsya naiti horoshie indikatory, kotorye pozvolili by na osnovanii sravneniya nablyudaemyh ostatkov s raschetnymi sdelat' vybor mezhdu razlichnymi mehanizmami vspyshki. Delo eto neprostoe. Poka postroena odnomernaya model'. Vryad li ona polnost'yu otrazhaet vsyu slozhnuyu kartinu vzryva i razleta obolochki.
Authors: J. Craig Wheeler
Comments: AAPT/AJP Resource Letter, American Journal of Physics, in press, 19 pages, 208 references
Bibliograficheskii obzor po sverhnovym. Ssylki razbity na neskol'ko tem: nablyudeniya spektrov, spektropolyarimetriya, krivye bleska, teoriya termoyadernyh vzryvov, kollaps yadra, radioaktivnyi raspad, kosmologicheskie prilozheniya, svyaz' s gamma-vspleskami.
Authors: L. Zampieri, et al.
Comments: 7 pages, 3 figures. MNRAS, in press
Sredi sverhnovyh vtorogo tipa - vzryvy massivnyh zvezd - nablyudaetsya dovol'no bol'shoi razbros svoistv. V chastnosti, est' bolee slabye sverhnovye. Avtory predstavlyayut dva primera takih vzryvov. I obsuzhdayut vozmozhnost' togo, chto takie vspyshki soprovozhdayutsya bol'shoi vozvratnoi akkreciei (fall-back). Sootvetstvenno, takie vzryvy dolzhny privodit' k obrazovaniyu chernyh dyr. Krome togo, stadiya akkrecii mozhet vposledstvii nablyudat'sya, kogda akkrecionnaya svetimost' nachnet dominirovat'.
Authors: Adam Burrows, Todd A. Thompson
Comments: 10 pages, LaTeX, 4 JPEGs included. To be published in the proceedings to the ESO/MPA/MPE Workshop (an ESO Astrophysics Symposium) entitled "From Twilight to Highlight: The Physics of Supernovae," held in Garching bei M\"unchen, Germany, July 29-31, 2002, eds. Bruno Leibundgut and Wolfgang Hillebrandt (Springer-Verlag)
Obsuzhdaetsya sovremennyi status neitrinnyh modelei vzryvov sverhnovyh. Eto samaya standartnaya i naibolee prodvinutaya model' vzryva v rezul'tate kollapsa yadra massivnoi zvezdy. Rassmatrivayutsya problemy modeli i avtorskie popytki ih preodoleniya.
Authors: Schuyler D. Van Dyk et al.
Comments: 19 pages, 23 figures, to appear in PASP (2003 Jan)
Odna iz problem v astrofizike sverhnovyh zvezd - ponyat' kakie zvezdy kakie sverhnovye porozhdayut. Dlya etogo hotelos' by imet' izobrazhenie zvezdy do vzryva. Avtory predstavlyayut rezul'taty poiskov takih dannyh. Arhivy Kosmicheskogo teleskopa i drugih proektov pozvolili obnaruzhit' praroditelei neskol'kih sverhnovyh raznyh tipov (konechno, rech' ne idet o sverhnovyh tipa Ia). Est' ukazaniya na obnaruzhenie shesti zvezd, kotorye zatem vzorvalis'. SN II porozhdayutsya krasnymi sverhgigantami. S SNe Ib/c ne vse tak yasno.
Authors: V. Belokurov, N.W. Evans
Comments: 9 pages, 4 figures, MNRAS, to appear
"Super-Hipparcos" - eto budushii astrometricheskii sputnik GAIA. Ego zapusk planiruetsya na 2010 god. Srok raboty sputnika - 5 let. Sputnik budet poluchat' horoshuyu mnogocvetnuyu fotometriyu. T.o. v rukah issledovatelei okazhetsya kolossal'noe kolichestvo informacii. Seichas aktivno obsuzhdayutsya razlichnye "pobochnye" produkty raboty GAIA.
V dannoi rabote avtory obsuzhdayut, chto sputnik smozhet dat' dlya astrofiziki sverhnovyh zvezd. Ocenki pokazyvayut, chto za 5 let sputnik smozhet zaregistrirovat' bolee 20 000 sverhnovyh (pyat' v den')! Primerno dve treti - eto sverhnovye Ia. V osnovnom eto blizkie (Z<0.14). Otdel'no avtory obsuzhdayut vozmozhnost' registracii gamma-izlucheniya i gravitacionnyh voln ot sverhnovyh, zamechennyh GAIA.
Authors: R. Napiwotzki, N. Christlieb, H. Drechsel, H.-J. Hagen, U. Heber, D. Homeier, C. Karl, D. Koester, B. Leibundgut, T.R. Marsh, S. Moehler, G. Nelemans, E.-M. Pauli, D. Reimers, A. Renzini, L. Yungelson
Commets: in: "From Twilight to Highlight", eds. W. Hillebrandt & B. Leibundgut, ESO Astrophysics Symposia, Springer-Verlag, in press, 6 pages, 2 figures Report-no: RP-21-02
Soglasno odnomu iz scenariev vspyshka sverhnovoi tipa Ia proishodit v rezul'tate sliyaniya dvuh dostatochno massivnyh belyh karlikov. Poisk takih sistem velsya v eksperimente SPY (SN Ia Progenitor surveY). V hode kotorogo na teleskope VLT s pomosh'yu spektrometra UVES iskalis' izmeneniya luchevyh skorostei. Otkryto 90 novyh dvoinyh belyh karlikov, vklyuchaya korotkoperiodicheskie sistemy s massami komponent blizkimi k chandrasekarovskomu predelu.
Authors: M.Turatto, S.Benetti, E.Cappellaro
Commets: 10 pages, 4 figues, to appear in Proc. "From Twilight to Highlight - The Physics of Supernovae" ESO/MPA/MPE Workshop Garching July 29 - 31, 2002
V nachale kazhetsya, chto zhenshiny delyatsya na blondinok i bryunetok. Potom zamechaesh', chto est' shatenki i voobshe ottenki. Potom vydelyaesh' krashenyh blondinok, bryunetok, shatenok i t.d. T.e. "ponimanie prihodit s opytom" .... Tak zhe i so sverhnovymi.
Do 80-h godov vydelyali dva tipa sverhnovyh. No chem bol'she nablyudali, tem bol'she ponimali, chto etogo nedostatochno. V svoem korotkom obzore avtory rasskazyvayut o mnogoobrazii sverhnovyh. Formul net, est' grafiki, krivye bleska i t.p. Nu i, konechno zhe, ssylki na original'nye raboty.
Authors: Avishay Gal-Yam et al.
Commets: 25 pages, 2 figures, To appear in AJ, Feb. 2003 issue
V rezul'tate vypolneniya programmy poiska sverhnovyh obnaruzheny 7 sverhnovyh tipa Ia v skopleniyah galaktik na z ot 0.06 do 0.2, ne prinadlezhashie ni k odnoi iz galaktik skopleniya. Veroyatno eti zvezdy ne byli vybrosheny iz galaktik, a rodilis' iz diffuznogo gaza, zapolnyayushego mezhgalakticheskoe prostranstvo. Avtory predpolagayut, chto okolo 20% sverhnovyh v skopleniyah galaktik mogut okazat'sya mezhgalakticheskimi.
Authors: Neil Gehrels et al
Commets: 24 pages, 4 Postscript figures, to appear in The Astrophysical Journal, 2003 March 10, vol. 585
Rassmotreno vozdeistvie vspyshki blizkoi sverhnovoi na ozonovyi sloi Zemli. Avtory pokazali, chto blizkaya (<8 pk) sverhnovaya svoim zhestkim izlucheniem mozhet umen'shit' soderzhanie ozona v 2 raza na srok v neskol'ko let. Proishodit eto iz-za rezkogo uvelicheniya v atmosfere soderzhaniya molekul oksidov azota, kotorye intensivno reagiruyut s ozonom i razrushayut ego. Chastota takih vspyshek ocenivaetsya v 1.5.10-9 let-1.
Authors: Christofer Gunnarsson and Ariel Goobar (Stockholm University)
Commets: 9 pages, 16 figures, submitted to A&A
Skoplenie galaktik na z~0.3-0.5 mozhet sdelat' sushestvenno yarche raspolozhennuyu za nim sverhnovuyu. Na skol'ko? Kak chasto eto budet proishodit'? V kakom fil'tre ih luchshe nablyudat'? Eti i ryad drugih voprosov rassmotreny v dannoi stat'e.
Authors: Adam Burrows, Todd A. Thompson
Commets: 46 pages, including 9 figures. To be published as a Chapter in "Core Collapse of Massive Stars," ed. C.L. Fryer, Kluwer Academic Publ
Bol'shaya poluobzornaya rabota na styke nauk. Avtory dayut obzor po vzaimodeistviyu neitrino s veshestvom pri parametrah, sootvetstvuyushih kollapsiruyushemu yadru sverhnovoi. Stat'ya dovol'no special'naya, a potomu vryad li budet interesna ochen' shirokoi publike. Odnako, ona mozhet byt' interesna fizikam, kotorye redko soprikasayutsya s astrofizikoi.
Authors: S. T. Holland (Notre Dame)
Commets: 12 pages, 7 figures, uses econfmacros.tex, to appear in the NBSI conference proceedings for Beaming and Jets in Gamma-Ray Bursts
V stat'e dan korotkii obzor opticheskih poslesvechenii gamma-vspleskov. Rassmotrena kak klassicheskaya model' faerbola, tak i ryad al'ternativnyh modelei ("pushechnogo yadra", zaderzhannogo vzryva).
Authors: Shizuka Akiyama, J. Craig Wheeler
Commets: 18 pages, 4 figures. To appear in conference proceedings "Core Collapse of Massive Stars," ed. C. L. Fryer, Kluwer Academic Pub
V principe yasno, chto magnitnye polya dolzhny igrat' bol'shuyu rol' pri vzryve sverhnovoi. Svyazano eto ne tol'ko (i ne stol'ko) s tem, chto vo vzryvayusheisya zvezde uzhe bylo pole, a eshe i s faktom generacii polya pri kollapse. Odnako, raschety vseh etih processov ochen' slozhny. My i bez ucheta polya kak sleduet poschitat' sverhnovuyu ne mozhem (raschety takih vzryvov po vsei vidimosti yavlyayutsya odnoi iz samyh slozhnyh sovremennyh schetnyh zadach).
V stat'e krome svoih original'nyh rezul'tatov avtory dayut dovol'no horoshii obzor sostoyaniya del v dannoi oblasti, privodya okolo 70 ssylok (v osnovnom na detal'nye raschety).
Authors: S. Feltzing, T. Bensby, I. Lundstrom (Lund Observatory, Sweden)
Commets: 4 pages, 3 figures, A&A Letter in press
Kak mozhno uznat', chto v dannom meste kogda-to vzorvalas' sverhnovaya, esli dazhe ee ostatok uzhe ischez? Po raspredeleniyu dostatochno molodyh zvezd i gradientu himicheskogo sostava. Stat'ya posvyashena poisku staryh vspyshek sverhnovyh tipa Ia i sravneniyu vozrastov tonkogo i tolstogo diskov na etoi osnove.
Authors: Chris L. Fryer, Daniel E. Holz, Scott A. Hughes, and Michael S. Warren
Commets: 31 pages, 9 figures, to appear in "Stellar Collapse" (Astrophysics and Space Science), edited by C. L. Fryer Report-no: NSF-KITP-02-174, LAUR-02-6960
Vse blizhe i blizhe moment, kogda s nazemnyh gravitacionnyh antenn nachnut postupat' eksperimental'nye dannye (oni uzhe est', tol'ko v nebol'shom kolichestve). I nado uspet' predskazat', chto mozhno v nih uvidet'. V etom obzore osnovnoe vnimanie obrasheno na gravitacionnye volny ot kollapsov yader sverhnovyh.
Authors: V. N. Gamezo et al.
Commets: 17 pages, 5 figures. To appear in Science, January 2003
V meru populyarnaya i polnaya stat'ya (material idet v Science) po sverhnovym tipa Ia, t,e, po vzryvam belyh karlikov. No krasivyh kartinok malo - vsego odna stranichka (9-ya).
Authors: Dong Lai
Commets: Conference proceedings; to be published in "Radio Pulsars" (ASP Conf. Ser.), ed. M. Bailes, D. Nice, & S. Thorsett. 7 pages
My ploho znaem: kak vzryvayutsya sverhnovye. Sootvetstvenno, my ploho predstavlyaem svoistva novorozhdennyh kompaktnyh ob'ektov, naprimer, neitronnyh zvezd. Avtor daet spisok nereshennyh problem, osobenno podrobno obsuzhdaya problemu skorostei otdachi (kick velocity) neitronnyh zvezd. Prostoi ponyatnyi obzorchik.
Authors: H.-Th. Janka et al.
Commets: 34 pages; 11 figures. Review for ore Collapse of Massive Stars'', Ed. C.L. Fryer, Kluwer, Dordrecht
Podrobnyi kriticheskii obzor po mehanizmam vspyshek sverhnovyh. Rassmatrivayutsya vzryvy massivnyh zvezd. Zdes' sushestvuet eshe mnozhestvo nereshennyh problem (hotya, est' i drugie mneniya, Virdzhiniya Trimbl v svoem doklade na tehasskom simpoziume skazala, chto na ee vzglyad v celom problema reshena - ostalos' utochnit' detali). Tem ne menee, sformirovalas' "standartnaya kartina", kotoraya, pravda, mozhet eshe ochen' sil'no izmenit'sya. Avtory opisyvayut detal'nye dvumernye raschety i dayut sootvetstvuyushii background.
Sm. takzhe bolee korotkie obzory teh zhe avtorov: astro-ph/0212316 i astro-ph/0212317, i stat'yu "The Status of Core-collapse Supernova Simulations" astro-ph/0212438.
Authors: Christian Y. Cardall (Oak Ridge National Laboratory and University of Tennessee, Knoxville)
Commets: Contribution to the proceedings of the 4th International Workshop on the Identification of Dark Matter (IDM2002), held in York, England 2-6 September 2002, to be published by World Scientific. 10 pages, 1 figure
Izuchaya razlichnymi sposobami vzryvy sverhnovyh mozhno poluchat' ochen' raznoobraznuyu informaciyu - ot zakona rasshireniya Vselennoi i svoistv temnoi materii do uravneniya sostoyaniya neitronnogo veshestva i sushestvovaniya ekzoticheskih chastic. No dlya etogo nado horosho ponimat' kakie processy v nih proishodyat. I edinstvennyi put' zdes' - detal'noe chislennoe modelirovanie. No do segodnyashnego dnya pri modelirovanii kollapsa i vzryva sverhnovoi uchityvalis' ne vse fizicheskie processy - prosto potomu, chto dlya takih raschetov ne hvatilo by moshnosti komp'yuterov. TeraScale Supernova Initiative - proekt v kotorom v blizhaishie neskol'ko let predpolagaetsya preodolet' eti ogranicheniya.
Authors: E.N.Alexeyev, L.N.Alexeyeva
Commets: latex, 7 pages, 2 eps figures, JETP, vol.95, pp.5-10 (2002)
V stat'e summiruyutsya rezul'taty 20 let raboty Baksanskogo neitrinnogo teleskopa. Krome vspyshki sverhnovoi 1987A nikakih drugih vspleskov obnaruzheno ne bylo. Eto pozvolyaet dat' vazhnoe ogranichenie na temp poyavleniya sverhnovyh v nashei Galaktike: rezhe chem 0.13 v god.
Authors: S. Blinnikov, E. Sorokina
Commets: 16 pages, 7 figures; invited talk at the JENAM-2002 meeting (Porto, Portugal, September, 3-8)
Sverhnovye tipa Ia stali teper' "ob'ektami osoboi znachimosti" v svyazi s tem, chto oni ispol'zuyutsya v kosmologii kak standartnye svechi. V stat'e daetsya nebol'shoi obzor po etim sverhnovym, a zatem predstavlyayutsya novye original'nye rezul'taty po modelirovaniyu krivyh bleska etih istochnikov.
Authors: Mario Hamuy (OCIW)
Commets: 26 pages, 15 figures, Review for `Core Collapse of Massive Stars'', Ed. C.L. Fryer, Kluwer, Dordrecht
Daetsya podrobnyi i ponyatnyi obzor svoistv sverhnovyh, gde, kak polagayut, imel mesto kollaps yadra massivnoi zvezdy (tipy II, Ib,c). Avtor obrashaet osoboe vnimanie na to, chto pri vsem raznoobrazii nablyudatel'nyh proyavlenii svoistva etogo fenomena menyayutsya nepreryvno i, sledovatel'no, mehanizm vzryva u vseh sverhnovyh etogo klassa dolzhen byt' odinakov. Sm. takzhe nizhe astro-ph/0301107.
Authors: Massimo Turatto
Commets: 16 Pages, 4 figures, to be published in "Supernovae and Gamma-Ray Bursters," ed. Kurt W. Weiler
Opisyvaetsya sovremennaya klassifikaciya sverhnovyh.
Vo mnogom stat'ya pereklikaetsya s
astro-ph/0301006,
potomu luchshe chitat' ih vmeste (vozmozhno takzhe budet interesno posmotret'
nedavnii obzor po mehanizmam vzryvov massivnyh zvezd
astro-ph/0212314 i sverhnovyh tipa Ia
astro-ph/0212530).
obzor
astro-ph/0301334
Fizika sverhnovyh Ia i kosmologiya
(Physics of SNeIa and Cosmology)
Author: P. Hoeflich, C. Gerardy, E. Linder & H. Marion
Commets: 25 pages, to be published in "Stellar Candles", eds. Gieren et al.
Lecture
Notes in Physics (
http://link.springer.de/series/lnpp)
Obzor po sverhnovym tipa Ia i ih kosmologicheskim prilozheniyam.
Tri stat'i po sverhnovym i vzaimodeistviyu sverhnovyh s okruzhayushei sredoi
Authors: A. Jorissen, M. Dedecker, B. Plez, D. Gillet, A. Fokin
Commets: 8 pages, 6 figures. To appear in 'Journees Miras 2002', edited by M.O. Mennessier et al., Universite de Montpellier-II (2003). Also available at http://www-astro.ulb.ac.be/Html/ps.html#Tomo
Korrelyaciya spektra zvezdy s cifrovoi maskoi sinteticheskogo spektra pozvolyaet vydelit' v ee atmosfere sloi s povyshennoi svetimost'yu i/ili plotnost'yu. Metod pozvolyaet obnaruzhivat' udarnye fronty v atmosfere. Obsuzhdayutsya rezul'taty poluchennye dlya peremennyh zvezd RT Cyg i RY Cep otnosyashihsya k Miridam.
Authors: Roger A. Chevalier
Commets: 10 pages, to appear in Proc. "From Twilight to Highlight - The Physics of Supernovae" ESO/MPA/MPE Workshop, Garching July 2002
Sverhnovye vzryvayutsya ne v pustote. Vo-pervyh est' mezhzvezdnoe veshestvo, a
vo-vtoryh massivnaya zvezda imeet moshnyi veter.
T.o. dlya togo, chtoby ponyat', kak formiruyutsya ostatki sverhnovyh, neobhodimo
uchityvat' "blizhaishee okruzhenie" vzryvayusheisya zvezdy.
V nebol'shom obzore avtor rassmatrivaet razlichnye tipy sverhnovyh, svyazannye
s massivnymi zvezdami s tochki zreniya ih vzaimodeistviya s okolozvezdnym
veshestvom.
Authors: S. E. Woosley, A. Heger
Commets: 12 pages, 2 figures, to appear in Proc. IAU 215 "Stellar Rotation"
Raschety sverhnovyh stanovyatsya vse bolee i bolee prodvinutymi.
Teper' v standartnoi modeli vzryva nauchilis' uchityvat' vrashenie.
Ob etom i idet rech' v dannom korotkom obzore. Takzhe rassmatrivaetsya svyaz'
sverhnovyh s gamma-vspleskami.
Authors: A. Heger et al.
Commets: 10 pages, 2 figures, to appear in Proc. IAU 215 "Stellar Rotation"
Eta stat'ya samym neposredstvennym obrazom svyazana s predydushei, no eto ne obzor, a original'naya rabota dvuh grupp, ob'edinivshih svoi usiliya, dlya togo chtoby razobrat'sya s nachal'nym tempom vrasheniya neitronnyh zvezd. V itoge poluchayutsya dostatochno bystrovrashayushiesya neitronnye zvezdy: bez magnitnogo polya odni gidrodinamicheskie neustoichivosti i konvekciya ne mogut otodvinut' novorozhdennyi pul'sar ot vrasheniya na predele razrusheniya. Vliyanie magnitnogo polya uvelichivaet nachal'nyi period na poryadok (do 4-7 millisekund). V poslednem sluchae energii vrasheniya okazyvaetsya nedostatochno dlya togo, chtoby "zapitat'" gamma-vsplesk v modeli kollapsara. Odnako, "mnogoe sdelano, no mnogoe eshe predstoit". V chastnosti, v tesnyh dvoinyh sistemah situaciya mozhet sushestvenno otlichat'sya kak v tu, tak i v inuyu storonu.
Authors: Yong-Zhong Qian
Commets: 47 pages including 11 figures, invited review to appear in Progress in Particle and Nuclear Physics
Odna iz samyh vazhnyh problem, rassmatrivaemyh v shkol'nom kurse astronomii - eto proishozhdenie elementov. Otnyud' ne dlya vseh yavlyaetsya ochevidnym tot fakt, chto fakticheski kazhdyi atom nashego tela (krome, mozhet byt', vodoroda) kogda-to pobyval v nedrah zvezdy. Raznye elementy obrazuyutsya v razlichnyh processah. V obzore rassmatrivaetsya t.n. r-process - process bystrogo (rapid) neitronnogo zahvata (est' eshe medlennyi - slow - s-process). Obzor dovol'no bol'shoi i podrobnyi. Privoditsya massa ssylok na original'nye i obzornye raboty.
Sm. takzhe "Stellar Sources for Heavy r-Process Nuclei" astro-ph/0301461.
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: Weidong Li et al.
Commets: 60 pages, 12 figures. A high resolution PostScript version is available at http://astro.berkeley.edu/~weidong/sn2002cx.ps
"Dlya horoshego cheloveka nichego ne zhalko!" - 60 stranic o samoi neobychnoi sverhnovoi Ia.
V stat'e privodyatsya detal'nye dannye nablyudenii. Vyvod avtorov ochen' interesnyi: "Ni odna iz sushestvuyushih teoreticheskih modelei ne mozhet odnovremenno ob'yasnit' vse osobennosti sverhnovoi SN 2002cx".
Authors: D. A. Green, F. R. Stephenson
Commets: 12 pages, 4 figures, to be published in "Supernovae and Gamma Ray Bursters", ed. K. W. Weiler, Lecture Notes in Physics, Springer-Verlag, Berlin-Heidelberg-New York
Opisyvayutsya dannye po izvestnym istoricheskim (t.e. nablyudavshimsya nevooruzhennym glazom) sverhnovym: sverhnovaya Keplera, sverhnovaya Tiho, sverhnovye 1181, 1054 i 1006 gg. Sovetuem prochest' vsem. Chtenie legkoe i priyatnoe.
Authors: Arieh Koenigl
Commets: 8 pages, invited review, to appear in Gamma Ray Bursts in the Afterglow Era -- Third Workshop (Rome, September 2002), ASP Conference Series
Kratko opisyvaetsya model' supranovoi. V etoi modeli posle vzryva obrazuetsya massivnaya zamagnichennaya neitronnaya zvezda, kotoraya podderzhivaetsya bystrym vrasheniem. Zamedlenie privodit k kollapsu v chernuyu dyru. Model' primenyatesya dlya ob'yasneniya svoistv gamma-vspleskov. Esli eshe ne slyshali o takoi modeli - sovetuyu prochitat'.
Authors: F. Mannucci et al.
Commets: A&A, in press, 13 pages
Kak izvestno, v nashei galaktike sverhnovye ne nablyudalis' poslednie 400 let. I eto pri tempe vspyshek poryadka odnoi v 30 let! Ob'yasnenie prostoe - vspyhivayut daleko i zakryty pyl'yu. T.e. nesmotrya na potryasayushuyu moshnost' vzryva ego taki mozhno nezametit'. Pohozhaya kartina proishodit i v drugih galaktikah. Pravda, tam my redko vidim galaktiku s rebra, kak v sluchae Mlechnogo Puti, v ploskosti kotorogo my nahodimsya. Tem ne menee v galaktikah s burnym zvezdoobrazovaniem, gde dolzhno byt' mnogo sverhnovyh, mnogo i pyli. Poetomu interesno smotret' v IK diapazone, gde pyl' ne tak meshaet. Avtory predstavlyayut rezul'taty svoih issledovanii. Po nablyudeniyam 46 yarkih IK galaktik na dline volny 2.2 mikrona bylo otkryto 4 sverhnovye. Etot temp vspyshek primerno na poryadok prevoshodit temp opticheski zaregistrirovannyh vspyshek (otmetim, chto oshibki vse-taki veliki, t.k. statistika mala). Prichem, ozhidalos' eshe bol'she vspyshek. Znachit, kakie-to sverhnovye vse-taki "nagluho" zakryty pyl'yu....
Authors: Lifan Wang, Gerson Goldhaber, Greg Aldering, Saul Perlmutter (LBNL)
Commets: ApJ, in press
Vnimatel'noe rassmotrenie pochti lineinogo povedeniya krivyh bleska Sverhnovyh tipa Ia na diagramme cvet-zvezdnaya velichina (B - B-V ili B-R, ili B-I) pozvolyaet luchshe uchityvat' pogloshenie ih izlucheniya i proizvodit' korrekciyu ih svetimosti. Eto dostatochno sushestvenno, t.k. imenno eti sverhnovye sluzhili "standartnymi svechami" po kotorym opredelili, chto nasha Vselennaya rasshiryaetsya uskorenno.
Authors: R. Buras et al.
Commets: 5 pages, PRL submitted; 3 eps figures, 1 colored, high-quality available upon request
Na t.n. tehasskoi konferencii vo Florencii v dekabre poshlogo goda porazil kommentarii Virdzhinii Trimbl, chto v obshem-to problema vzryva sverhnovoi reshena Vusli, Viverom i dr. (plyus kak obychno ehidnyi kommentarii, chto esli vy ne otlichaete Vusli-Vivera ot Visli-Vuvera, to slishkom dolgo rabotaete v etoi oblasti). Po ee mneniyu, ostaetsya tol'ko uchityvat' tonkosti: pole, vrashenie, him.sostav i t.d.
Odnako, ne vse tak prosto. Gruppa Yanki i dr. davno vyskazyvala pessimizm otnositel'no sushestvuyushih problem v fizike vzryva sverhnovoi, po ih mneniyu slishkom mnogoe zakladyvaetsya rukami. Vot novoe podtverzhdenie ih vzglyadov.
Novye detal'nye dvumernye raschety s vrasheniem i bez ne dayut vzryva. Odnimi neitrino vrode kak ne oboitis'. Vozmozhno kritichen uchet magnitnyh polei ili kakoi-to ekzotiki.
O neitrino v sverhnovyh sm. takzhe otdel'nuyu stat'yu toi zhe gruppy "Supernova neutrinos: Flavor-dependent fluxes and spectra" astro-ph/0303226.
Authors: Saul Perlmutter, Brian P. Schmidt
Commets: In Supernovae & Gamma Ray Bursts, K. Weiler, Ed., Springer, Lecture Notes in Physics (in press), 24 pages, 7 figs
Dovol'no polnoe izlozhenie togo, kak po sverhnovym opredelyayut kosmologicheskie
parametry. Razbirayutsya (kratko) vse vozmozhnye istochniki neopredelennostei.
Mnogo (bolee 100) ssylok.
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