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

Mezhzvezdnaya sreda
(Arhiv Mezhzvezdnaya sreda:
v.2, 2003, v.1, 2002-2003)

Vypusk 202. 17-31 dekabrya 2008

arxiv:0812.3491 Uzor spiral'nyh rukavov Mlechnogo Puti (The Milky Way spiral arm pattern)
Authors: Peter Englmaier et al.
Comments: 6 pages, to appear in Mem.SAI

Po dannym nablyudenii molekulyarnogo gaza (SO) avtory stroyat trehmernuyu kartu Galaktiki, prorisovyvaya spiral'nye rukava. Vidny dva rukava, nachinayushiesya u bara vo vnutrennei chasti Galaktiki. Krome togo, vo vnutrennei chasti est' eshe para rukavov. Zatem eti rukava perehodyat v chetyrehrukavnuyu strukturu, nablyudayushuisya v linii neitral'nogo vodoroda vo vneshnih chastyah Galaktiki. Vpervye udalos' prosledit' spiral'nye rukava v oblasti za centrom Galaktiki.

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


Vypusk 201. 01-16 dekabrya 2008

obzor arxiv:0812.0046 Obzor kompleksa v Orione (Overview of the Orion complex)
Authors: John Bally
Comments: 26 pages, to be published in the Handbook of star formation regions, Vol. 1 Astronomical society of the Pacific, 2008, Ed. Bo Reiputh

Vyhodit zamechatel'nyi sbornik statei, v kotorom opisyvayutsya razlichnye oblasti zvezdoobrazovaniya. Prakticheski vse stat'i iz sbornika dostupny v Arhive. Ocherednaya poyavivshayasya stat'ya posvyashena blizhaishei oblasti zvezdoobrazovaniya v Orione, v kotoroi i seichas obrazuyutsya massivnye i malomassivnye zvezdy. Krome opisaniya sobstvenno kompleksa zvezdoobrazovaniya v Orione avtor dostatochno detal'no opisyvaet odin iz scenariev formirovaniya poyasa Gulda, i voobshe kartinu nedavnego zvezdoobrazovaniya v solnechnoi okrestnosti. Ochen' interesno i poznavatel'no.


arxiv:0812.0505 Modelirovanie Mestnogo teplogo/goryachego Puzyrya (Modeling the Local warm/hot Bubble)
Authors: Dieter Breitschwerdt et al.
Comments: 8 pages, to appear in the proceedings of @The Local Bubble and Beyond. II"

Avtory opisyvayut (ves'ma kratko, eto zhe materialy konferencii) svoyu novuyu chislennuyu model' formirovaniya i evolyucii Mestnogo Puzyrya, osnovannuyu na novyh nablyudatel'nyh dannyh. Puzyr' nachal formirovat'sya pochti 15 millionov let nazad. V etom "prinimali uchastie" 19 sverhnovyh, poslednyaya iz kotoryh rvanula primerno polmilliona let nazad. Eto byli zvezdy iz podgruppy B1 Pleyad. V budushem Puzyr' budet pogloshen obrazovaniem Loop I, kotoroe bylo porozhdeno 39 sverhnovymi (razumeetsya, chislo vzryvov - eto model'nyi parametr i tam est' nekotoraya neopredelennost'), svyazannymi s associaciei Skorpion-Centavr.


item obzor arxiv:0812.1448 Proishozhdenie i priroda pyli v rannei vselennoi (Origin and Nature of Dust in the Early Universe).
Authors: Takaya Nozawa et al.
Comments: 19 pages, 7 figures and 1 table. Submitted to the ASP conference proceedings of "Cosmic Dust - Near and Far"

Avtorami obzora prosummirovany poslednie dostizheniya v teoreticheskom izuchenii processov formirovaniya i evolyucii pyli v pervyh sverhnovyh, rassmatrivaemyh kak naibolee veroyatnyh istochnikah pyli v rannei vselennoi. Rassmotreny rezul'taty raschetov formirovaniya pyli v sverhnovyh zvezdah Pop III i evolyucii pyli v ostatkah sverhnovyh. Proanalizirovano, pochemu na bol'shih krasnyh smesheniyah mezhzvezdnyi gaz harakterizuetsya ploskoi krivoi ekstinkcii.


item arxiv:0812.1578 Soderzhanie zheleza v planetarnyh tumannostyah Galaktiki (The Iron Abundance in Galactic Planetary Nebulae).
Authors: G. Delgado-Inglada et al.
Comments: ApJ, 15 pages

Avtorami izucheno soderzhanie zheleza v 33 planetarnyh tumannostyah Galaktiki. Eto naibolee polnoe issledovanie na etu temu, poskol'ku ostaetsya nemalo voprosov o tom, skol'ko pyli soderzhitsya v etih ob'ektah. Analiz nablyudatel'nyh dannyh, provedennyi v rabote, pokazal, chto do 90 procentov atomov zheleza v planetarnyh tumannostyah kondensiruetsya v pyl'.


Vypusk 199. 01-13 noyabrya 2008

arxiv:0811.1552 O prirode HESS J1503-582 po dannym eksperimenta H.E.S.S.: sovpadenie s FVW? )On the nature of HESS J1503-582 revealed by the H.E.S.S. experiment: coincidence with a FVW?)
Authors: M. Renaud et al.
Comments: 4 pages

H.E.S.S. - nazemnaya sistema gamma-teleskopov. Odna iz ochen' rezul'tativnyh programm etogo proekta - obzor ploskosti Galaktiki. Pri etom bylo otkryto mnozhestvo istochnikov. Chast' iz nih udalos' otozhdestvit' s izvestnymi ob'ektami (ostatki sverhnovyh, pul'sary, tesnye dvoinye sistemy i tp.), a chast' - net. Istochnik J1503-582 - odin iz neotozhdestvlennyh. Nichego osobenno primechatel'nogo iz chisla obychnyh gamma-istochnikov tam ne obnaruzheno. Avtory obsuzhdayut lyubopytnuyu vozmozhnost'. Istonik sovpadaet s t.n. forbidden-velocity-wing. FVW - eto gazovaya struktura, nablyudaemaya v radiodiapazone, vydelyayushayasya svoei "Nepravil'noi" skorost'yu.


Vypusk 197. 13-19 oktyabrya 2008

obzor arxiv:0810.2923 Galakticheskie i vnegalakticheskie magnitnye polya (Galactic and extragalactic magnetic fields)
Authors: Rainer Beck
Comments: 14 pages, 14 figures, to be published in "High energy gamma-ray Astronomy"

Horoshii obzor po magnitnym polyam. Mnogo fakticheskih dannyh, illyustracii i ssylok. Formul net - odna fenomenologiya. Chitaetsya legko.


obzor arxiv:0810.2984 Perspektivy izucheniya zvezdnoi evolyucii i smerti v eru JWST (Prospects for studies of stellar evolution and stellar death in the JWST era)
Authors: Michel J. Barlow
Comments: 24 pages, 19 figures, to appear in "Astrophysics on the next decade: JWST and concurrent facilities"

Dovol'no bol'shoi obzor, posvyashennyi tomu, chto my smozhem uznat' v blizhaishie gody o rozhdenii, zhizni i smerti zvezd s pomosh'yu takih teleskopov kak Herschel, SOFIA, JWST.


Vypusk 196. 01-12 oktyabrya 2008

miniobzor arxiv:0810.0441 Geliosfera vo vremeni (The Heliosphere in Time)
Authors: H-R. Muller et al.
Comments: 12 pages, to appear in Space Science Reviews

Geliosfera postoyanno izmenyaetsya, poskol'ku Solnce proletaet skvoz' mezhzvezdnuyu sredu s raznymi parametrami. Izmenyayutsya svoistva sredy - plotnost', temperatura, skorost' otnositel'no Solnca - "dyshit" geliosfera. Avtory obsuzhdayut kakoi mogla byt' geliosfera v proshlom i kakoi mozhet stat' v budushem. Vse eti izmeneniya "galakticheskoi pogody" mogut imet' sovsem neakademicheskoe znachenie! Ispol'zuya dannye radionablyudenii, avtory delayut vyvod, chto bolee 9 procentov vremeni Solnce provodit v teploi neitral'noi (ili chastichno ionizovannoi) srede.


Vypusk 195. 12-30 sentyabrya 2008

arxiv:0809.1942 Obrazovanie GMO putem agglomeracii i za schet samogravitacii (GMC formation by agglomeration and self gravity)
Authors: Clare Dobbs
Comments: 16 pages, 12 figures, accepted for publication in MNRAS.

GMO - gigantskie molekulyarnye oblaka. Kak oni obrazuyutsya tochno ne izvestno. Vidimo rabotaet neskol'ko mehanizmov. V dannoi stat'e s pomosh'yu chislennogo modelirovaniya issleduyutsya dva iz nih.

Komp'yuternye simulyacii pokazali, chto pri nizkoi poverhnostnoi plotnosti gaza GMO obrazuyutsya v udarnyh volnah, svyazannyh so spiral'noi strukturoi, putem agglomeracii. T.e., otnositel'no nebol'shie sgustki gaza obrazuyut strukturu bol'shogo masshtaba. Pri vysokoi poverhnostnoi plotnosti gaza stanovitsya vazhnoi samogravitaciya. I GMO obrazuyutsya v rezul'tate razvitiya gravitacionnoi neustoichivosti. V nashei Galaktike plotnost' gaza takova, chto kak raz nachinaet dominirovat' gravitacionnaya neustoichivost'.

Avtor podrobno perechislyaet, chto ne bylo uchteno v modeli. V itoge vse-taki sozdaetsya oshushenie, chto: "Mnogoe sdelano, no mnogoe eshe predstoit."


Vypusk 189. 24 iyunya - 08 iyulya 2008

obzor arxiv:0807.0857 Organicheskoe veshestvo v kosmose (Organic Matter in Space - an Overview)
Authors: E.F. van Dishoeck
Comments: Introductory overview lecture presented at IAU Symposium 251, "Organic matter in space", held at Hong Kong, February 2008; to appear in IAU Symposium 251 proceedings, Cambridge University Press, ed. S. Kwok et al

Nebol'shoi ponyatno napisannyi obzor po organicheskim molekulam v kosmose (ot solnechnoi sistemy do dal'nih ugolkov galaktiki). Opisano chto i kak nablyudayut, i kak ono moglo obrazovat'sya.


Vypusk 188. 10-23 iyunya 2008

miniobzor arxiv:0806.1673 Itogi konferencii: izuchenie neitral'nogo vodoroda v sleduyushem desyatiletii (Conference Summary: HI Science in the Next Decade)
Authors: Martha P. Haynes
Comments: To appear in AIP Conference Proceedings, "The Evolution of Galaxies through the Neutral Hydrogen Window", Feb 1-3 2008, Arecibo, Puerto Rico, eds. R. Minchin & E. Momjian. 8 pages

V Arhive potihon'ku poyavlyayutsya stat'i, kotorye budut opublikovany v materialah konferencii po izucheniyu neitral'nogo vodoroda. Eti issledovaniya vazhny dlya ponimaniya processa formirovaniya galaktik, nekotoryh kosmologicheskih aspektov.

O proekte ALFALFA (The Arecibo Legacy Fast ALFA) mozhno prochest' tut arxiv:0806.1670. V ego ramkah provoditsya obzor vnegalakticheskogo neitral'nogo vodoroda (razumeetsya, rech' idet o volne 21 sm). Na nastoyashii moment zakoncheno bolee poloviny nablyudatel'noi raboty i okolo chetverti raboty po obrabotke dannyh.

Ob istorii i rezul'tatah issledovaniya blizkih galaktik na volne 21 sm sm. arxiv:0806.1712. Razumeetsya, na radioteleskope v Aresibo, kotoryi seichas igraet vedushuyu rol' v issledovanii galaktik na volne 21sm, planiruyutsya novye nablyudeniya. Pro to napisano zdes' arxiv:0806.1714.


Vypusk 176. 20 dekabrya 2007-09 yanvarya 2008 goda

arxiv:0712.4264 Trehmernoe raspredelenie molekulyarnogo gaza v Galaktike s uchetom bara (3D Distribution of Molecular Gas in the Barred Milky Way)
Authors: Martin Pohl, Peter Englmaier, Nicolai Bissantz
Comments: 27 pages, ApJ in press

Predstavlena novaya model' trehmernogo raspredelenie molekulyarnogo gaza v nashei Galaktike. Avtory ispol'zuyut i dannye po izlucheniyu molekuly SO, i dannye chislennogo modelirovaniya, i nekotoruyu druguyu informaciyu. Vazhno, chto model' budet dostupna dlya skachivaniya.


Vypusk 174. 01-13 dekabrya 2007

obzor arxiv:0712.0954 Chislennoe modelirovanie turbulentnosti (The Numerical Simulation of Turbulence)
Authors: W. Schmidt
Comments: 18 pages, 7 figures; proceedings contribution to "Structure formation in the Universe: Chamonix 2007"

Nebol'shoi obzor, posvyashennyi dostatochno populyarnomu izlozheniyu togo, kak modeliruyut turbulentnost' voobshe, a v osobennosti v sluchae mezhzvezdnoi sredy.


Vypusk 173. 20-30 noyabrya 2007

miniobzor arxiv:0711.4047 Obratnaya svyaz' (v obrazovanii massivnyh zvezd): teoreticheskii obzor (Feedback Processes [in Massive Star Formation]: A Theoretical Perspective)
Authors: Mordecai-Mark Mac Low (
Comments: for publication in the proceedings of "Massive Star Formation: Observations Confront Thoery", ASP conference series, eds. H. Beuther et al., 10 pages

Esli vy hotite uznat', kak mnogo my eshe ne ponimaem v voprose formirovaniya massivnyh zvezd, i skol' veliko kolichestvo obsuzhdaemyh interesnyh idei, to vam syuda.

Avtor daet obzor po sleduyushei probleme: chto opredelyaet maksimal'nuyu massu zvezd. Po vsei vidimosti, verhnii predel na massu zvezd v kazhdom konkretnom sluchae opredelyaetsya summarnym deistviem mnogih faktorov, kotorye vse svyazany s "obratnoi svyaz'yu". T.e., chem massivnee obrazuyushayasya zvezda, tem bol'she ona izluchaet, tem sil'nee veter i istecheniya, chto, v svoyu ochered', prepyatstvuet dal'neishemu uvelicheniyu massy.

Obsudiv mnozhestvo mehanizmov (zamechu, chto v osnovnom ssylki na raboty 2006-2007 goda, t.o., vse "s pylu s zharu"), avtor rezyumiruet, chto my vse-taki poka ne ponimaem, chto opredelyaet maksimal'nuyu massu zvezdy.

Sm. takzhe obzor po obrazovaniyu massivnyh zvezd arxiv:0711.4912.


Vypusk 172. 01-19 noyabrya 2007

item arxiv:0711.0005 Absorbciya O VI v diske Galaktiki po nablyudeniyam sputnika FUSE (The Far Ultraviolet Spectroscopic Explorer Survey of O VI Absorption in the Disk of the MilkyWay).
Authors: David V. Bowen et al.
Comments: ApJ S, 105 pages

Poskol'ku soderzhanie kisloroda v mezhzvezdnoi srede veliko, a dublet linii O VI 1032, 1037A udoben dlya nablyudenii v ul'trafioletovom diapazone, pyatikratno ionizovannyi kislorod OVI yavlyaetsya horoshim indikatorom raspredeleniya goryachego mezhzvezdnogo gaza s temperaturoi T= 3 x 105 K. Samyi prostoi sposob poiska absorbcionnyh linii OVI - eto monitoring goryachih zvezd rannih klassov O2-B3, yavlyayushihsya yarkimi ul'trafioletovymi istochnikami. Avtory raboty izuchili absorbcionnye spektry 148 zvezd, poluchennye s pomosh'yu sputnika FUSE. Po rezul'tatam izmerenii naideno, chto srednyaya koncentraciya atomov O VI v diske Galaktiki sostavlyaet poryadka n= 1-3 x 10-8 cm-3 i eksponencial'no ubyvaet s rasstoyaniem ot galakticheskoi ploskosti.


item arxiv:0711.1093 Issledovanie CO v galaktikah na z = 0.4 - 1.5 (CO investigation of z = 0.4 - 1.5 galaxies).
Authors: A.L. Melchior & F. Combes
Comments: A&A, 6 pages

Dannaya rabota posvyashena poisku emisionnyh linii molekul CO v treh galaktikah, nahodyashihsya na krasnyh smesheniyah ot 0.4 do 1.5. Nablyudeniya provodilis' na radioteleskope IRAM-30m. Sut' raboty sostoyala v tom, chtoby issledovat' soderzhanie molekulyarnogo vodoroda v galaktikah, aktivno izluchayushih v infrakrasnom diapazone. Odnako ni v odnoi iz galaktik-kandidatov zafiksirovat' sushestvennogo kolichestva molekulyarnogo vodoroda avtoram ne udalos'.


item arxiv:0711.1372 Poisk predvestnikov zhizni v dalekih galaktikah (Searching for the Precursors of Life in External Galaxies).
Authors: B. Lawton et al.
Comments: conf. proceedings, 6 pages

Rabota posvyashena poisku organicheskih molekul v udalennyh galaktikah. Esli ta ili inaya galaktika nahoditsya mezhdu nablyudatelem i kvazarom, popadaya na luch zreniya na kvazar, to galaktika ostavit svoi "otpechatki" v absorbcionnom spektre kvazara. V chastnosti, takim sposobom mozhet byt' opredelen himicheskii sostav ee mezhzvezdnoi sredy. Slozhnye organicheskie molekuly proyavlyayut sebya v vide diffuznyh polos poglosheniya. Avtory raboty popytalis' naiti i izuchit' diffuznye polosy v absorbcionyh spektrah kvazarov. Slozhnye organicheskie molekuly, bezuslovno, ne mogut rassmatrivat'sya kak zhizn', no oni predstavlyayut opredelennyi interes dlya astrobiologii.

V ramkah proekta bylo otobrano neskol'ko galaktik s bol'shim soderzhaniem neitral'nogo vodoroda, nazyvaemyh nasyshennymi laiman-al'fa sistemami (damped Ly-alpha systems). Rezul'taty pokazali, chto dlya poiska diffuznyh polos takaya iznachal'naya selekciya bednyh metallami i pyl'yu galaktik ne yavlyaetsya effektivnoi. Soderzhanie organicheskih molekul v DLA-galaktikah nedostatochno, chtoby byt' zafiksirovannym sovremennymi priborami.


item arxiv:0711.1588 Zhizn' za chertoi: zvezdoobrazovanie i himicheskaya evolyuciya ekstremal'no bogatoi gazom galaktiki (Life in the last lane: Star formation and chemical evolution in an extremely gas-rich dwarf).
Authors: A. Begum et al.
Comments: MNRAS, 9 pages

V rabote priveden analiz nablyudatel'nyh dannyh po karlikovoi irregulyarnoi galaktike NGC 3741. Izuchiv raspredelenie neitral'nogo vodoroda HI, izobrazhenie v linii H_alpha i soderzhanie kisloroda v mezhzvezdnoi srede, avtory prishli k vyvodu, chto NGC 3741 predstavlyaet soboi protyazhennyi gazovyi disk (8.8 radiusov Holmberga). Polnaya massa neizluchayushei materii prevyshaet zvezdnuyu v 149 raz, tem ne menee otnoshenie barionov k samoi temnoi materii tipichno dlya etogo klassa galaktik. U galaktiki sformirovan central'nyi bar i est' protyazhennaya gazovaya spiral'naya vetv'. NGC 3741 evolyucioniruet ochen' medlenno. Srednii temp zvezdoobrazovaniya sostavlyaet 0.0034 solnechnyh mass/god. Po ocenke avtorov, NGC 3741 ne sil'no otlichaetsya ot drugih karlikovyh irregulyarnyh galaktik, poskol'ku naidennye parametry yavlyayutsya tipichnymi.


item arxiv:0711.1843 Poisk diffuznyh polos v spektrah obolochek post-AGB zvezd (A search for diffuse bands in the circumstellar envelopes of post-AGB stars).
Authors: R. Luna et al.
Comments: A&A, 25 pages

Priroda diffuznyh polos poglosheniya ostaetsya nereshennoi problemoi fiziki mezhzvezdnoi sredy. V opticheskom i infrakrasnom diapazonah sovremennye katalogi naschityvayut uzhe bolee dvuhsot takih polos, no vopros, kakie imenno molekuly otvetstvenny za pogloshenie, ostaetsya otkrytym. Naibolee veroyatnymi kandidatami nazyvayut slozhnye ogranicheskie molekuly. Sushestvuet principial'naya raznica mezhdu polosami poglosheniya, formiruyushimisya v diffuznoi MZS i v protyazhennyh obolochkah post-AGB zvezd. Fizicheskie usloviya (plotnost', uroven' ionizacii, himicheskii sostav gaza) v etih sluchayah sovershenno razlichny. Opisat' sostoyanie diffuznoi MZS na osnove nablyudenii chasto ochen' trudno, zato opredelit' sostav gaza i pyli v obolochkah post-AGB zvezd v poslednie gody stalo vozmozhnym. Nablyudeniya diffuznyh polos poglosheniya v atmosferah post-AGB zvezd (esli oni tam est'!) mogli by proyasnit' obshii mehanizm formirovaniya diffuznyh polos v MZS. Imenno etoi celi posvyashena dannaya rabota.

Nablyudeniya provodilis' v techenie 1993-2003 gg na teleskopah WHT 4.2m, TNG 3.58m, VLT 8m, NTT 3.5m, ESO 1.52m. Avtorami byli polucheny spektry vysokogo razresheniya dlya 33 post-AGB zvezd v opticheskom intervale dlin voln 4000-10000 A. Tipichnoe vremya ekspozicii sostavilo okolo poluchasa, otnoshenie S/N 20-200. Cel'yu nablyudenii byl poisk devyati naibolee sil'nyh difuznyh polos poglosheniya na dlinah voln 5780, 5797, 5850, 6196, 6284, 6379, 6614, 6993 i 7224 A. Ni odnoi iz devyati polos v obolochkah 33 post-AGB zvezd obnaruzheno ne bylo. Razdelenie zvezd na gruppy v zavisimosti ot spektral'nogo klassa i himicheskogo sostava obolochki (uglerodnye ili kislorodnye zvezdy) takzhe ne pozvolilo vyyavit' kakoi-libo korrelyacii. Po mneniyu avtorov, diffuznye polosy v obolochkah post-AGB zvezd libo otsutstvuyut voobshe, libo slishkom slaby dlya togo, chtoby ih mozhno bylo zafiksirovat' sovremennymi priborami. Himicheskii sostav zvezdnyh obolochek i usloviya, otlichnye ot tipichnyh uslovii v diffuznoi MZS, veroyatno, privodyat k tomu, chto molekuly, vyzyvayushie diffuznye polosy, v atmosferah post-AGB zvezd prosto ne formiruyutsya.


item arxiv:0711.2166 Solnechnoe obilie indiya (On the solar abundance of indium).
Authors: N. Vitas et al.
Comments: MNRAS, 7 pages

Indii - himicheskii element s rekordnym otlichiem solnechnogo i meteoritnogo obilii. Meteoritnoe znachenie sostavlyaet A(In)=0.8 +/- 0.03, v to vremya kak soderzhanie indiya v solnechnoi fotosfere na 0.8 dex bol'she. Chtoby ob'yasnit' raznicu, avtory raboty zanovo rassmotreli metodiku nahozhdeniya solnechnogo obiliya. Analiz pokazal, chto liniya 4511.3 A, obychno rassmatrivaemaya kak liniya In I, vyzvana otnyud' ne indiem, a drugim, ne indentificirovannym poka elementom (predpolozhitel'no, ionom s vysokoi energiei vozbuzhdeniya). Uchet etih popravok privodit k horoshemu soglasiyu mezhdu solnechnym i meteoritnym soderzhaniem indiya, ustranyaya vyshenazvannoe protivorechie.


Vypusk 171. 17-31 oktyabrya 2007

item arxiv:0710.2997 Vliyanie oblakov galakticheskogo vetra na evolyuciyu bogatyh gazom karlikovyh galaktik (The effect of clouds in a galactic wind on the evolution of gas-rich dwarf galaxies)
Authors: S. Recchi1 & G. Hensler
Comments: A&A, 13 pages

Bogatye gazom karlikovye galaktiki podrazdelyayut na karlikovye irregulyarnye nizkoi poverhnostnoi yarkosti (dIrr), i yarkie golubye karlikovye galaktiki (BCD). I te, i drugie imeyut nizkuyu metallichnost' i slozhnuyu mnogokomponentnuyu gazovuyu strukturu. Ih mezhzvezdnaya sreda sostoit iz holodnoi, teploi i goryachei diffuznoi faz. Avtory dannoi raboty issledovali, kak uchet holodnyh oblakov povliyaet na dinamicheskuyu i himicheskuyu evolyuciyu karlikovyh galaktik. Rezul'taty modelirovaniya sravnivalis' avtorami s ih zhe rezul'tatami, no poluchennymi v ramkah standartnogo obsheprinyatogo podhoda. Chislennye eksperimenty pokazali, chto uchet holodnoi oblachnoi fazy umen'shaet teplovuyu energiyu MZS na 20-40%, chto sushestvenno umen'shaet veroyatnost' obrazovaniya krupnomasshabnyh istechenii. Obshaya metallichnost' MZS karlikovoi galaktiki pri etom ponizhaetsya na 0.2-0.4 poryadka dex, hotya otnositel'nye soderzhaniya elementov ostayutsya prezhnimi.


item arxiv:0710.3340 Rasstoyanie do vysokoskorostnyh oblakov Galaktiki. Kompleks C (Distances to Galactic high-velocity clouds. Complex C)
Authors: B.P. Wakker et al.
Comments: ApJ Let, 12 pages

Evolyuciya galaktik polnost'yu opredelyaetsya kolichestvom mezhzvezdnogo gaza. Chem bol'she gaza, tem bolee prodolzhitel'na evolyuciya. Strogoi granicy mezhdu galaktikami i mezhgalakticheskoi sredoi ne sushestvuet, proishodit postoyannyi obmen. Obogashennyi metallami gaz pokidaet galaktiku v vide galakticheskogo vetra, a nizkometallichnyi gaz akkreciruetsya iz mezhgalakticheskoi sredy. Nalichie akkrecii gaza s nizkim soderzhaniem tyazhelyh elementov kosvenno sleduet iz modelei himicheskoi evolyucii, poskol'ku nalichie akkrecii neobhodimo dlya ob'yasneniya obshirnogo nablyudatel'nogo materiala. Neposredstvennym dokazatel'stvom popolneniya Galaktiki gazom sluzhit sushestvovanie vysokoskorostnyh oblakov (VSO) - protyazhennyh oblakov neitral'nogo gaza, imeyushih skorost' poryadka 100 km/s otnositel'no Galaktiki. Avtory dannoi raboty proanalizirovali rasstoyanie do sistemy oblakov "kompleks S". Dannaya stat'ya - prodolzhenie ih rabot na etu temu (k primeru, astro-ph 0709.1926). Sut' metoda prosta: v napravlenii vysokoskorostnogo oblaka vybirayutsya zvezdy, rasstoyaniya do kotoryh izvestny s horoshei tochnost'yu. Ocenku rasstoyaniya do oblaka mozhno poluchit', izuchaya linii mezhzvezdnogo poglosheniya v spektrah etih zvezd. Nablyudeniya provedeny avtorami v observatoriyah McDonald, Keck i WHT. V rabote ispol'zovany dannye radionablyudenii. Po mneniyu avtorov, rasstoyanie do oblaka "kompleks S" nahoditsya v predelah ot 3.7 kpk (po drugoi ocenke 6.7 kpk) do 11.2 kpk. Ocenka rasstoyaniya provedena vpervye. Bol'shoi interval v neskol'ko kiloparsek svyazan kak s protyazhennost'yu samogo oblaka, imeyushego bol'shoi uglovoi diametr, tak i s neobhodimost'yu utochneniya etogo rezul'tata s pomosh'yu dal'neishih nablyudenii. Metallichnost' "kompleksa S" sostavlyaet 15% ot solnechnoi. Izmerenie kolichestva neitral'nogo vodoroda vdol' oblaka po luchu zreniya pozvolilo ocenit' massu neitral'nogo vodoroda. Nablyudenii v linii H_alpha pokazali, chto soderzhanie neitral'nogo i ionizovannogo gaza v oblake primerno odinakovy. Obshaya ocenka massy oblaka sostavila 3.-14. x 106 solnechnyh mass, chto sootvetstvuet tempu akkrecii 0.1-0.25 mass Solnca/god. Obshii temp akkrecii mezhgalakticheskogo gaza Galaktikoi ocenivaetsya kak 1 massa Solnca/god, potomu vklad oblaka "kompleks S" sostavlyaet ot 10 do 25%. Rasstoyanie do vysokoskorostnyh oblakov ostavalos' zagadkoi dolgoe vremya. Sovremennye nablyudeniya pokazyvayut, chto VSO nahodyatsya v predelah galo Galaktiki, a ih nizkaya metallichnost' i napravlenie dvizheniya podtverzhdayut tot fakt, chto Galaktika na protyazhenii vsei evolyucii nepreryvno "podpityvaetsya" gazom izvne. Zadachei posleduyushih issledovanii budet postroenie trehmernoi karty raspredeleniya VSO.


Vypusk 170. 01-16 oktyabrya 2007

item arxiv:0710.0901 Diffuznye polosy v spektrah absorbiruyushih sistem CaII na krasnyh smesheniyah z < 0.6 (Diffuse Interstellar Bands in z < 0.6 CaII Absorbers).
Authors: Sara Ellison1 et al.
Comments: MNRAS, 5 pages

Priroda diffuznyh linii poglosheniya (diffuse bands) ostaetsya odnoi iz nereshennyh zadach spektroskopii. Proshozhdenie ih svyazano s nekimi mehanizmami poglosheniya v mezhzvezdnoi srede, poskol'ku intensivnost' etih linii chetko korreliruet s velichinoi mezhzvezdnogo poglosheniya E(B-V) i koncentraciei neitral'nogo vodoroda na luche zreniya N(HI). V Galaktike i Magellanovyh Oblakah diffuznye linii poglosheniya nablyudayutsya na dlinah voln 4428, 5705, 5780, 5797, 6284, 6613 A. Naibolee veroyatnym ob'yasneniem diffuznyh polos schitayut slozhnye organicheskie molekuly. Tak nazyvaemye absorbcionnye sistemy Ca II - eto udalennye galaktiki, kotorye nablyudayutsya tol'ko v liniyah poglosheniya v spektrah kvazarov. Oni kak raz harakterizuyutsya bol'shim soderzhaniem neitral'nogo vodoroda N(HI) i sushestvennym znacheniem E(B-V). Eti sistemy mogut byt' polezny v kachestve instrumenta izucheniya diffuznyh linii poglosheniya na kosmologicheskih rasstoyaniyah, i tem samym dlya izucheniya svoistv mezhzvezdnoi sredy v dalekih galaktikah.

V dannoi rabote predprinyata imenno takaya popytka. Na teleskope VLT byli provedeny nablyudeniya 9 absorbcionnyh sistem CaII (galaktik), nahodyashihsya na krasnyh smesheniyah 0.07 < zabs < 0.55. Diffuznaya polosa na 5780 A byla detektirovana tol'ko dlya odnoi galaktiki, nahodyasheisya na krasnom smeshenii z=0.1556 v napravlenii kvazara J0013-0024. Eto vtoroi izvestnyi sluchai obnaruzheniya diffuznoi linii poglosheniya na kosmologicheskom rasstoyanii. V predpolozhenii galakticheskih svoistv mezhzvezdnoi sredy, avtory ocenili, chto dlya etoi galaktiki soderzhanie neitral'nogo vodoroda prevyshaet logN(H I) > 20.9 sm-2, a E(B-V)=0.23 mag. Eti ocenki kosvenno podtverzhdayut obshee predstavlenie o sistemah CaII kak galaktikah, imeyushih naibol'shuyu sredi absorbcionnyh sistem N(H I) i zapylennost'. Perspektivy dal'neishih nablyudenii avtory svyazyvayut imenno s etimi sistemami, hotya s nablyudatel'noi tochki zreniya eto predstavlyaet soboi ochen' slozhnuyu zadachu. Ekvivalentnaya shirina linii 5780 A dlya galaktiki s E(B-V) = 0.1 mag sostavlyaet vsego 30 mA, a eto men'she sovremennogo predela detektirovaniya v 2-3 raza. Poetomu obnaruzhenie diffuznyh polos poglosheniya naibolee veroyatno tol'ko v absobcionnyh sistemah s naibol'shim soderzhaniem pyli.


item arxiv:0710.1062 Novyi vzlyad na soderzhanie zheleza v gazovoi faze (New Insights on Interstellar Gas-Phase Iron).
Authors: A. Jensen & T. Snow
Comments: ApJ, 53 pages

Zhelezo - odin iz samyh rasprostranennyh v prirode tyazhelyh elementov. V mezhzvezdnoi srede atomy zheleza soderzhatsya v osnovnom v tverdoi (pylevoi) faze. Dlya kolichestvennogo opisaniya stepeni kondensacii atomov togo ili inogo elementa iz gazovoi v pylevuyu fazu vvedeno ponyatie deplecii. Eto logarifm otnosheniya polnogo kolichestva atomov dannogo elementa k kolichestvu atomov v gazovoi faze. Uvelichenie deplecii neizbezhno oznachaet rost chisla atomov, pereshedshih v tverduyu fazu. Nablyudaemye variacii znacheniya deplecii zavisyat ot uslovii v mezhzvezdnoi srede i mogut byt' kosvennoi harakteristikoi ee sostoyaniya. Avtory raboty prosummirovali dannye nablyudenii FUSE (Far Ultraviolet Spectroscopic Explorer) i HST (Hubble Space Telescope) dlya atomov odnokratno ionizovannogo zheleza (FeII). Soderzhanie zheleza v gazovoi faze mezhzvezdnoi sredy bylo izucheno imi dlya 51 napravlenii. Dlya etogo byli izmereny ekvivalentnye shiriny absorbcionnyh linii zheleza, a zatem ego soderzhanie naideno metodom krivyh rosta. Na osnove bol'shogo statisticheskogo materiala avtorami byli podtverzhdeny naidennye ranee korrelyacii mezhdu depleciei zheleza i polnoi luchevoi koncentraciei vodoroda, usrednennoi ob'emnoi plotnost'yu vodoroda, dolei molekulyarnogo vodoroda, ekstinkciei i drugimi harakteristikami. Nekotorye iz perechislennyh v stat'e zavisimostei obnaruzheny vpervye. Issledovanie dlya drugogo himicheskogo elementa - magniya - predstavleno avtorami v rabote arxiv:0710.1064.


item arxiv:0710.1303 Absorbcionnye spektry gamma-vspleskov kak test modelei reionizacii (Testing Reionization with Gamma Ray Burst Absorption Spectra).
Authors: Gallerani et al
Comments: MNRAS, 5 pages

Dlinnye gamma-vspleski (GRB) na bol'shih krasnyh smesheniyah mogut stat' odnim iz effektivnyh testov teorii reionizacii. Na segodnya izvestno uzhe pyat' ochen' dalekih gamma-vspleskov na z > 5, rekordnyi iz kotoryh GRB 050904 nahoditsya na krasnom smeshenii z=6.29. Spektry dalekih kvazarov i gamma-vspleskov harakterizuyutsya glubokimi provalami (gaps) levee linii Ly-alpha, priroda kotoryh sostoit v tom, chto vse izluchenie v etoi oblasti pogloshaetsya neitral'nym vodorodom na luche zreniya mezhdu istochnikom i nablyudatelem. Statistika takih "provalov" v spektrah dalekih kvazarov nedavno byla priznana effektivnym sredstvom izucheniya ionizacionnogo sostoyaniya mezhgalakticheskoi sredy (MGS). Absorbcionnye spektry ochen' dalekih gamma-vspleskov tak zhe mogut byt' ispol'zovany dlya etoi celi, no oni imeyut svoyu osobuyu specifiku. Prezhde vsego sama priroda kvazarov i gamma-vspleskov sushestvenno razlichna. Poslesvechenie gamma-vspleskov ubyvaet so vremenem, potomu nablyudeniya MGS v napravlenii gamma-vspleska v razlichnye dni poslesvecheniya predstavlyaet dopolnitel'nuyu vozmozhnost' izucheniya vremennoi evolyucii "provalov" i pozvolyaet otobrat' naibolee realistichnye modeli reionizacii. Tak, avtory predskazyvayut, chto esli reionizaciya zakonchilas' pozzhe, to "provaly" v absorbcionnyh spektrah gamma-vspleskov na z > 6 budut shire i gorazdo mnogochislennee. Predstavlennyi v rabote podhod imeet bol'shie preimushestva. Ozhidaetsya, chto v blizhaishem budushem budut otkryty gamma-vspleski na z > 6 i chto takih nablyudenii budet mnogo. Eto pozvolit znachitel'no uluchshit' statisticheskii analiz i vosstanovit' istoriyu reioniacii v detalyah.


item arxiv:0710.2225 Sostav pyli v galakticheskom vetre kvazara PG 2112+059 (Dust in the wind: Crystalline silicates, corundum and periclase in PG 2112+059)
Authors: F. Markwick-Kemper et al.
Comments: ApJ, 14 pages

Mineralogicheskii sostav pyli, prinadlezhashei kvazaru PG 2112+059, byl detal'no izuchen avtorami s pomosh'yu dannyh, poluchennyh kosmicheskim teleskopom Spitzer. Analiz spektra kvazara v infrakrasnom diapazone i popytka vosproizvesti ego posredstvom modelirovaniya pokazali nalichie bogatyh magniem amorfnyh silikatov (56.5+/-.4)%, a takzhe prisutstvie Al2O3 (38+/-)% i MgO (2.7+/-1.7)%. Hotya formirovanie pyli proishodit v atmosferah zvezd i ostatkah sverhnovyh, nablyudaemye v sluchae kvazara PG 2112+059 svoistva pylevyh chastic ne isklyuchayut vozmozhnosti dal'neishei akkumulyacii pyli v galakticheskom vetre samogo kvazara.


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.

item arxiv:0709.2974 Istechenie ili galakticheskii veter: sud'ba ionizovannogo gaza v galo karlikovyh galaktik (Outflow or galactic wind: The fate of ionized gas in the halos of dwarf galaxies)
Authors: J. van Eymeren et al.
Comments: 15 pages, A&A in press

Nablyudeniya karlikovyh galaktik v emissionnyh liniyah vyyavili mnogochislennye struktury ionizovannogo gaza na rasstoyaniyah do kiloparseka ot oblastei zvezdoobrazovaniya. Eti struktury okaimlyayut bol'shie gruppy massivnyh zvezd, nazyvaemye OB-associaciyami. Vzryvy sverhnovyh i intensivnyi zvezdnyi veter peredayut energiyu massivnyh zvezd okruzhayushei mezhzvezdnoi srede. Obrazuyushiesya vokrug OB-associacii puzyri (superbubble) goryachego gaza, rasshiryayas', vymetayut okruzhayushii gaz. Tonkie plotnye obolochki takih "puzyrei" horosho razlichimy na opticheskih snimkah v emissionnyh liniyah. Karlikovye galaktiki sravnitel'no malomassivny, poetomu voznikaet vopros o dal'neishei sud'be ionizovannogo gaza. Budet li on gravitacionno svyazan s galaktikoi (v literature etot variant izvesten kak outflow - istechenie) ili sumeet preodolet' gravitacionnyi bar'er i navsegda pokinet galaktiku v vide galakticheskogo vetra (galactic wind)? Otvet na etot vopros vazhen dlya ponimaniya himicheskoi evolyucii galaktik i processov obogasheniya mezhgalakticheskoi sredy tyazhelymi elementami. Esli gaz pokidaet galaktiku, zvezdoobrazovanie v nei na kakoe-to vremya prekrashaetsya, a metallichnost' mezhzvezdnoi sredy umen'shaetsya. S tochki zreniya teorii, galakticheskii veter horosho izuchen i aktivno ispol'zuetsya v modelyah dinamicheskoi i himicheskoi evolyucii galaktik, no ubeditel'nye primery takih nablyudenii poka privesti trudno. Interpretaciyu dannyh uslozhnyaet uchet nevidimoi temnoi materii v galo galaktik, raspredelenie i massa kotoroi ne do konca yasny. Chislennoe znachenie skorosti "ubeganiya", dostigaya kotoruyu gaz mozhet pokinut' galaktiku, neodnoznachno, poskol'ku zavisit ot prinyatoi modeli temnoi materii. S cel'yu vyyasnit' svyazan ili net gravitacionno ionizovannyi gaz, nablyudaemyi okolo irregulyarnyh karlikovyh galaktik NGC 2366 and NGC4861, avtorami raboty byli polucheny glubokie snimki galaktik v linii H_alpha. Naidennye mnogochislennye struktury ionizovannogo gaza (razmerom ot soten parsek do kiloparseka v diametre) byli detal'no issledovany s tochki zreniya kinematiki s pomosh'yu dlinnoshelevoi eshele-spektroskopii vysokogo razresheniya na 4-m teleskope Observatorii Kitt Pik. Analiz rezul'tatov pokazal, chto oblaka ionizovannogo gaza pokidayut obe galaktiki so skorostyami ot 20 and 110 km/c. Chtoby vyyasnit', imeet li mesto v dannom sluchae istechenie (outflow) ili galakticheskii veter (galactic wind), eti skorosti nuzhno bylo sravnit' so skorost'yu "ubeganiya", opredelyaemoi model'yu temnoi materii. Provedennoe avtorami sravnenie pokazalo, chto oboih sluchayah gaz gravitacionno svyazan s galaktikami. Po mneniniyu avtorov, dlya nablyudatel'nogo podtverzhdeniya idei galakticheskogo vetra nuzhno obratit'sya k menee massivnym galaktikam s men'shim gravitacionnym potencialom, a takzhe uvelichit' chuvstvitel'nost' nablyudenii, chto pozvolilo by detektirovat' bolee slaboe izluchenie ionizovannogo gaza v galo galaktik.


obzor arxiv:0709.3814 Molekuly v galaktikah (Molecules in galaxies)
Authors: Alain Omont
Comments: 96 pages, 11 figures, Rep. Prog. Phys. 70 (2007) 1099-1176

Podrobnyi obzor po "molekulam v drugih galaktikah". V drugih galaktikah my mozhem nablyudat' mezhzvezdnuyu sredu pri ochen' raznyh usloviyah. Razumeetsya, etot material gorazdo bogache togo, kotoryi my nahodim v nashei Galaktike. Krome togo, v blizhaishem budushem, blagodarya vvodu v stroi novyh insturmentov, kolichestvo i kachestvo nablyudenii v etoi obalsti eshe vozrastut. Ob etom takzhe idet rech' v obzore.


arxiv:0709.4480 Struktura mestnoi mezhzvezdnoi sredy. IV. Dinamika, morfologiya, fizicheskie svoistva i prilozheniya k vzaimodeistviyu mezhdu oblakami (The Structure of the Local Interstellar Medium IV: Dynamics, Morphology, Physical Properties, and Implications of Cloud-Cloud Interactions)
Authors: Seth Redfield, Jeffrey L. Linsky
Comments: 65 pages, 24 figures; Accepted for publication in ApJ

Na osnovanii dannyh po blizkim zvezdam (oni vystumayut v roli testerov, prosvechivayushih mezhzvezdnuyu sredu) predstavlena model' lokal'noi mezhzvezdnoi sredy. Rech' idet o masshtabah neskol'ko desyatkov parsek i men'she. Model' ochen' detal'naya, poetomu za podrobnostyami - v stat'yu.


Vypusk 168. 11-18 sentyabrya 2007

item arxiv:0709.1926 Rasstoyaniya do galakticheskih HVC (Distances to Galactic high-velocity clouds. I. Cohen Stream, complex GCP, cloud g1)
Authors: B.P. Wakker, et al.
Comments: Accepted by ApJ

Horosho izvestno, chto galaktiki - otkrytye sistemami. Oni aktivno akkreciruyut gaz iz mezhgalakticheskoi sredy ( HVC, IVC ) i vymetayut sobstvennyi mezhzvezdnyi gaz posredstvom galakticheskogo vetra ("galakticheskie fontany" i t.d.). Analiz etih processov, stol' vazhnyh dlya ponimaniya dinamicheskoi i himicheskoi evolyucii galaktik, nevozmozhen bez nablyudenii. S etoi cel'yu na VLT nablyudalis' 24 udalennye zvezdy Galaktiki s izvestnymi rasstoyaniyami. Analiz mezhzvezdnoi absorbcii na luche zreniya v spektrah etih zvezd pozvolil ocenit' diapazon rasstoyanii do interesnyh chetyreh oblakov s massami poryadka M~ 10^5 solnechnyh mass. Okazalos', chto oblako " Cohen Stream" nahoditsya na rasstoyanii ot 5.0-11.7 kps i vmeste s oblakom " complex GCP" (rasstoyanie 9.8-15.1 kps) dvizhetsya v napravlenii Galaktiki. Oblaka zhe "Fountain in Perseus Arm" (rasstoyanie 1.0-2.7 kps) i "cloud g1" (1.8-3.8 kps) yavlyayutsya galakticheskimi fontanami.


Vypusk 167. 25 avgusta - 10 sentyabrya 2007

miniobzor arxiv:0708.4175 Spitcerovskii vzglyad na planetarnye tumannosti (Spitzer's View of Planetary Nebulae)
Authors: Joseph L. Hora
Comments: 8 pages, 2 figures, invited review to appear in the proceedings of the conference "Asymmetrical Planetary Nebulae IV", eds. R.L.M. Corradi, A. Manchado & N. Soker

Nebol'shaya stat'ya, v kotoroi dana svodka dannyh po planetarnym tumannostyam, poluchennyh na kosmicheskom infrakrasnom teleskope imeni Spitcera.

Drugoi poleznyi korotkii obzor iz togo zhe sbornika (uzhe yasno, chto takim miniobzorov budet mnogo) posvyashen asimmetrii planetarnyh tumannostei.


arxiv:0709.0485 Rasstoyanie do tumannosti Oriona (The distance to the Orion Nebula)
Authors: K. M. Menten et al.
Comments: 13 pages, 3 figures, to appear in Astronomy & Astrophyiscs

S pomosh'yu VLBA izmeren trigonometricheskii parallaks dlya neskol'kih chlenov skopleniya v tumannosti Oriona. Rasstoyanie ravno 414+/-7 pk.


arxiv:0709.0750 Zakon poglosheniya i svoistva pyli v napravlenii Magellanovyh oblakov ( Reddening law and interstellar dust properties along Magellanic sight-lines)
Authors: Frederic Zagury
Comments: accepted for publication in Astrophysics and Space Science. 16 pages, 12 figures.

Provedennyi avtorom analiz nablyudatel'nyh dannyh pokazal, chto zakony poglosheniya v nashei Galaktike, Bol'shom i Malom Magellanovom oblakah imeyut odinakovuyu prirodu i, sledovatel'no, net neobhodimosti v predpolozhenii o tom, chto svoistva pylevyh chastic v etih galaktikah sil'no otlichayutsya drug ot druga. S tochki zreniya avtora sovremennyi uroven' znaniya ne pozvolyaet vydelit' i opisat' takie razlichiya.


Vypusk 164. 20-31 iyulya 2007

obzor arxiv:0707.3514 Teoriya obrazovaniya zvezd (Theory of Star Formation)
Authors: Christopher F. McKee, Eve C. Ostriker
Comments: 120 pages, to appear in ARAA.

Obsuzhdayutsya vse aspekty obrazovaniya zvezd.


Vypusk 163. 01-19 iyulya 2007

arxiv:0707.2252 O bystrom kollapse i evolyucii molekulyarnyh oblakov (On the Rapid Collapse and Evolution of Molecular Clouds)
Authors: Bruce G. Elmegreen
Comments: 46 pages, 5 figures, scheduled for ApJ 668, October 20, 2007

Bol'shaya rabota, v kotoroi podrobno rassmatrivaetsya kollaps, privodyashii k poyavleniyu zvezd v gigantskih molekulyarnyh oblakah.


Vypusk 154. 01-12 aprelya 2007

obzor arxiv:0704.0770 Himicheskaya evolyuciya (Chemical Evolution)
Authors: Francesca Matteucci
Comments: 56 pages, Lectures delivered at the XVIII Canarie Winter School on "Emission Lines Universe"

Ochen' detal'naya lekciya po himicheskoi evolyucii. Termin "himicheskaya evolyuciya" primenim, razumeetsya, v pervuyu ochered' ili k mezhzvezdnoi, ili k mezhgalakticheskoi srede. Vse eto v obzore est'. Est' tam eshe i opisanie razlichnyh processov, opredelyayushih etu evolyuciya. T.o., avtoru prihoditsya govorit' edva li ne o polovine vsei astrofiziki!


Vypusk 150. 15-28 fevralya 2007

astro-ph/0702410 Vliyanie magnitnogo polya na formirovanie odinochnyh i dvoinyh zvezd (The impact of magnetic fields on single and binary star formation)
Authors: Daniel J. Price, Matthew R. Bate
Comments: 15 pages, 12 figures, accepted for publication in MNRAS.

Avtory chislenno modelirovali process zvezdoobrazovaniya s uchetom vliyaniya magnitnyh polei. Rezul'taty raschetov neskol'ko otlichayutsya ot osnovnoi massy analogichnyh rabot, prodelannyh ranee. Rol' magnitnyh polei, po raschetam avtorov, okazyvaetsya ochen' velika. Magnitnoe davlenie sushestvenno prepyatstvuet fragmentacii molekulyarnogo oblaka. V chastnosti, sil'nye polya mogut prepyatstvovat' formirovaniyu tesnyh dvoinyh zvezdnyh sistem, a takzhe planetnyh sistem. Zato mogut obrazovyvat'sya shirokie dvoinye zvezdy (te. sistemy s bol'shim or'ital'nym periodom).


miniobzor astro-ph/0702596 Mestnyi puzyr' i mezhzvezdnoe veshestvo okolo Solnca (The Local Bubble and Interstellar Material Near the Sun)
Authors: P. C. Frisch
Comments: 12 pages, Proceedings of Symposium on the Composition of Matter, honoring Johannes Geiss on the occasion of his 80th birthday

Dano opisanie mezhzvezdnoi sredy i proishodyashih v nei processov dlya rastoyanii poryadka 100-200 parsek ot nas. V etoi oblasti nedavnie vspyshki sverhnovyh i moshnyi veter massivnyh zvezd priveli k poyavleniyu interesnyh struktur, kotorye my mozhem izuchat' v melkih detalyah, blagodarya blizkomu rasstoyaniyu. Samaya vazhnaya dlya nas struktura - eto Local Bubble t.e. Mestnyi puzyr'.

Na moi vzglyad, istoriya proishozhdeniya Mestnogo Puzyrya i Poyasa Gulda dany slishkom uzh bezappellyacionno. Tem ne menee, obzor zasluzhivaet vnimaniya.


Vypusk 143. 18-31 oktyabrya 2006

miniobzor astro-ph/0610558 Dvoinye zvezdy v planetarnyh tumannostyah (Binary central stars of planetary nebulae)
Authors: Albert A. Zijlstra
Comments: 8 pages, Invited review, in 'Evolution and chemistry of symbiotic stars and related objects', Wierzba, August 2006. To appear in Baltic Astronomy

Nebol'shoi, no ochen' emkii obzor. Kak chitatel' pomnit, ya ne raz rasskazyval o probleme formy planetarnyh tumannostei. O roli dvoistvennosti zvezd i o roli magnitnyh polei v etom voprose. Vse, chto kasaetsya dvoistvennosti summirovano v dannom obzore.

Dvoistvennost' mozhet vliyat' na formu tumannosti troyakim obrazom. Vo-pervyh, mozhet imet' mesto stadiya obshei obolochki. V etom sluchae nalichie kompan'ona privodit k ochen' sushestvennoi i bystroi poteri massy. Esli sistema bolee shirokaya, to kompan'on mozhet ne vliyat' na temp sbrosa veshestva, zato povliyaet na formu tumannosti. Nakonec, v sluchae samyh shirokih sistem iz-za smesheniya centra mass forma tumannosti takzhe okazhetsya ne takoi, kak u odinochnyh zvezd.

Yasno, chto dvoistvennost' vliyaet na formu planetarnoi tumannosti. No interesno, chto ostaetsya mnogo nereshennyh problem. Tak, naprimer, dlya mnogih tumannostei s ves'ma ekzoticheskoi formoi poka ne udaetsya poluchit' kakie-to dannyh o dvoistvennosti zvezd, ih porodivshih.


astro-ph/0610769 Trehmernoe raspredelenie mezhzvezdnoi sredy v Galaktike: II. Molekulyarnyi gazovyi disk (Three-Dimensional Distribution of the ISM in the Milky Way Galaxy: II. The Molecular Gas Disk)
Authors: Hiroyuki Nakanishi, Yoshiaki Sofue
Comments: 19 pages, 15 figures, 3 tables

Po radionablyudeniyam postroena trehmernaya karta raspredeleniya molekulyarnogo gaza v Galaktike. Horosho vidny spiral'nye rukava. Zametno takzhe, gde maksimumy v raspredelenii gaza lezhat ne v ploskosti Galaktiki.

Krasivo!


obzor astro-ph/0610810 Mezhplanetnaya i mezhzvezdnaya plazmennaya turbulentnost' (Interplanetary and interstellar plasma turbulence)
Authors: A. A. Schekochihin et al.
Comments: IOP latex, 16 pages, 1 figure; invited topical review at International Congress on Plasma Physics, Kiev 22-26 May 2006; accepted for publication in Plasma Phys. Control. Fusion

Dovol'no slozhnyi obzor po plazmennoi turbulentnosti v astrofizike (v kachestve prostogo populyarnogo vvedeniya sm. stat'i v "Fizike kosmosa" po turbulentnosti i plazmennoi turbulentnosti). Posvyashen on v pervuyu ochered' teorii, a ne nablyudeniyam.


Vypusk 141. 15-30 sentyabrya 2006

astro-ph/0609709 Inducirovannoe zvezdoobrazovanie v okrestnosti massivnyh molodyh zvezd (Triggered Star Formation in the Environment of Young Massive Stars)
Authors: M. Gritschneder, T. Naab, F. Heitsch, A. Burkert
Comments: 4 pages, 2 figures. To appear in: "Triggered Star Formation in a Turbulent ISM", IAU Symposium 237, Prague, Czech Republic, August 2006; eds. B.G.Elmegreen & J. Palous

S pomosh'yu chislennogo modelirovaniya avtory pokazyvayut, chto ioniziruyushee izluchenie massivnyh molodyh zvezd sposobno inducirovat' zvezdoobrazovanie v blizkih molekulyarnyh oblakah.


Vypusk 139. 01-31 avgusta 2006

miniobzor astro-ph/0608048 Peremezhaemost' magnitogidrodinamicheskoi teurbulentnosti: astrofizicheskii vzglyad (Intermittency of Magnetohydrodynamic Turbulence: Astrophysical Perspective)
Authors: A. Lazarian
Comments: 14 pages, 7 figures, invited lecture at Trieste, published in International Journal of Modern Physics 15 (2006) 1

Ocherednoi obzor Lazaryana po MGD turbulentnosti v astrofizike.


Vypusk 138. 01-31 iyulya 2006

astro-ph/0607638 Raspredelenie mezhzvezdnoi sredy v Mlechnom Puti. Trehmernaya krupnomasshtabnaya model' (The distribution of the ISM in the Milky Way A three-dimensional large-scale model)
Authors: A. Misiriotis et al.
Comments: 14 Pages, 10 figures

Po dannym nablyudenii v mikronnom diapazone na COBE/DIRBE avtory stroyat trehmernuyu kartinu raspredeleniya gaza i zvezd v Galaktike. Krome togo, polucheny ocenki raspredeleniya tempa zvezdoobrazovaniya po radiusu.


Vypusk 134. 12-21 aprelya 2006

astro-ph/0604427 Trehmernoe modelirovanie galakticheskogo mezhzvezdnogo poglosheniya (Modelling the Galactic Interstellar Extinction Distribution in Three Dimensions)
Authors: D.J. Marshall, A.C. Robin, C. Reyle, M. Schultheis, S. Picaud
Comments: 20 pages, 15 figures, accepted for publication in A&A.

S pomosh'yu t.n. 2-mikronnogo obzora neba (2MASS) avtory vosstanavlivayut trehmernoe raspredelenie mezhzvezdnogo poglosheniya v nashei Galaktike.


Vypusk 125. 18-20 yanvarya 2006

obzor astro-ph/0601356 Vvedenie: paleogeliosfera protiv paleoMMZS (Introduction: Paleoheliosphere versus PaleoLISM)
Authors: Priscilla C. Frisch
Comments: The article will appear in the book "Solar Journey: The Significance of Our Galactic Environment for the Heliosphere and Earth", Springer, in press (2006), editor P. C. Frisch

Glava iz knigi (sm. takzhe astro-ph/0601359).

MMZS - Mestnaya mezhzvezdnaya sreda. Obsuzhdaetsya, kak variacii MMZS mogut vliyat' na zemnoi klimat.

Vsem sovetuyu!!!!


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 112. 22-31 iyulya 2005

obzor astro-ph/0507686 Turbulenciya i magnitnye polya v astrofizicheskoi plazme (Turbulence and Magnetic Fields in Astrophysical Plasmas)
Authors: A. A. Schekochihin, S. C. Cowley
Comments: latex, 26 pages, 12 figures; an invited chapter in the book "Magnetohydrodynamics: Historical Evolution and Trends" edited by S. Molokov, R. Moreau and H. K. Moffatt, to be published by Springer

Obzor po astrofizicheskoi plazme. Nachinaetsya vse s istorii i osnov. Detal'no rassmotrena plazma solnechnogo vetra i mezhgalakticheskaya sreda v skopleniyah.


Vypusk 108. 20-31 maya 2005

miniobzor astro-ph/0505574 Astrofizicheskie prilozheniya turbulentnyh peresoedinenii: ot kosmicheskih luchei do zvezdoobrazovaniya (Astrophysical Implications of Turbulent Reconnection: from cosmic rays to star formation)
Authors: A. Lazarian
Comments: 12 pages, 3 figures, invited review for "Magnetic Fields in the Universe: from laboratory and stars to Primordial Structures

Poyavilos' srazu neskol'ko obzorov Lazaryana i ego kolleg, posvyashennyh mezhzvezdnoi tutrulentnosti. V dannom obsuzhdaetsya interesnyi process peresoedineniya magnitnyh silovyh linii za schet turbulentnosti mezhzvezdnogo gaza. Etot process mozhet sushestvenno vliyat' na processy uskoreniya kosmicheskih luchei, a takzhe na zvezdoobrazovanie.


Vypusk 102. 21-31 marta 2005

obzor astro-ph/0503569 Mezhzvezdnye pylevye chasticy - 75-letnii yubilei (Interstellar Grains -- The 75th Anniversary)
Authors: Aigen Li
Comments: invited review article for the "Light, Dust and Chemical Evolution" conference (Gerace, Italy, 26--30 September 2004), edited by F. Borghese and R. Saija, 2005, in press

Aigen Li vylozhil neskol'ko svoih obzorov, posvyashennyh mezhzvezdnoi pyli. Semidesyatipyatiletie, upomyanutoe v zagolovke svyazano so stat'ei Tryumplera 1930 g., gde vpervye dostoverno bylo pokazano nalichie mezhzvezdnoi pyli.

Drugie obzory togo zhe avtora - eto stat'i astro-ph/0503567 i astro-ph/0503271


Vypusk 97. 17-31 yanvarya 2005

astro-ph/0501466 Raspredelenie OVI na luche zreniya v Mestnom puzyre (Ovi Column Density Distribution in the Local Bubble - Results from 3D Adaptive Mesh Refinement Simulations)
Authors: Miguel A. de Avillez^(1,2) and Dieter Breitschwerdt
Comments: 3 Pages, 3 figures (including 1 jpg image and 3 plots); poster paper to appear in "Astrophysics in the Far Ultraviolet: Five Years of Discovery with FUSE", 2005, ASP Conference Series, eds. G. Sonneborn, H. W. Moos, and B-G Andersson

Kratko opisyvaetsya ocherednaya popytka chislenno promodelirovat' obrazovanie Mestnogo puzyrya. Rezul'taty pokazyvayut, chto poslednii vzryv proizoshel 0.4-1.1 milliona let nazad, a naibolee blizkii k Solncu imel mesto 2.1-3.5 milliona let nazad.

Takzhe sm. stat'yu teh zhe avtorov astro-ph/0501586
Vypusk 92. 15-30 noyabrya 2004
obzor astro-ph/0411739 Vvedenie v galakticheskoe dinamo (Introduction to galactic dynamos)
Authors: Anvar Shukurov
Comments: 58 pages, 8 figures; to be published in "Mathematical Aspects of Natural Dynamos", EDP Press

Kak izvestno, vo Vselennoi magnitnye polya sushestvuyu na samyh raznyh masshtabah. Est', v tom chisle, i galakticheskoe magnitnoe pole. Ono kak-to bylo sozdano, i ego postoyanno neobhodimo podderzhivat'. Na segodnyashnii den' teoriya galakticheskogo dinamo s odnoi storony dostatochno horosho razrabotana, s drugoi - est' ryad nereshennyh voprosov. Obo vsem etom - v obzore Anvara Shukurova.


Vypusk 87. 01-10 oktyabrya 2004

astro-ph/0410109 Mikroarksekundnoe nebo kosmicheskaya turbulentnost'. (The Microarcsecond Sky and Cosmic Turbulence)
Authors: T. Joseph W. Lazio et al.
Comments: 20 pages, 8 figures

O tom, chto mezhzvezdnaya sreda turbulizovana, vsem davno i horosho izvestno, odnako do sih por nablyudeniya takoi turbulentnosti velis' tol'ko na ochen' bol'shih masshtabah. Kazhetsya v blizhaishem budushem, s poyavleniem SKA (antenny-v-kvadratnyi-kilometr) takaya vozmozhnost' poyavitsya. Ee razreshenie budet sostavlyat' millionnye doli uglovi sekundy, chto pozvolit razlichat' detali ot dolei astronomicheskih edinic do soten kilometrov(!).


Vypusk 86. 20-30 sentyabrya 2004

astro-ph/0409577 Pyl' ot sverhnovoi v dalekom kvazare (A supernova origin for dust in a high-redshift quasar)
Authors: R. Maiolino et al.
Comments: To Appear in Nature, September 30, 2004

Kak izvestno, uzhe na bol'shih krasnyh smesheniyah nablyudaetsya prakticheski solnechnyi himicheskii sostav veshestva. Krome togo nablyudaetsya i mezhzvezdnaya pyl'. Proishozhdenie ee do konca ne yasno, odnako naibolee ochevidnym kandidatom yavlyayutsya sverhnovye (drugoi variant - pozdnie stadii evolyucii zvezd).

Maiolino i dr. issledovali spektr kvazara na krasnom smeshenii z=6.2. Nablyudeniya provodilis' v IK diapazone na ital'yanskom teleskope im. Galileya.

Obrabotka dannyh pokazala, chto nablyudaemoe pogloshenie prekrasno opisyvaetsya modelyami, v kotoryh pyl' porozhdaetsya sverhnovymi tipa II, t.e. vzryvami massivnyh zvezd.


Vypusk 84. 01-12 sentyabrya 2004

miniobzor astro-ph/0409096 Poyas Gulda, zvezdoobrazovanie i lokal'naya mezhzvezdnaya sreda (The Gould Belt, star formation, and the local interstellar medium)
Authors: Isabelle A. Grenier
Comments: 10 pages, 4 figures

Istoriya lokal'noi mezhzvezdnoi sredy i lokal'nogo (zhe) zvezdoobrazovaniya na rasstoyanii do neskol'kih sot parsek i za period v neskol'ko desyatkov millionov let pochti polnost'yu opredelyaetsya poyasom Gulda. Avtor rassmatrivaet pochti vse: zony HI i H2, obrazovanie obychnyh i massivnyh zvezd, a iz poslednih - rentgenovskih istochnikov.


Vypusk 80. (01) - 12-20 iyunya 2004

astro-ph/0405167 Galakticheskie okrestnosti Solnca (The Solar Galactic Environment)
Authors: P.C.Frisch
Comments: 8 pages, 3 figures

Eta rabota, kak nazval ee avtor, "kombinirovannoe issledovanie" geliosfery (do 500AE) i blizhaishih mezhzvezdnyh okrestnostei (do 106AE) [Hotya, kak takoe mozhno skombinirovat'? Masshtaby razlichayutsya na 3 poryadka]. Dinamika oblakov podtverzhdaet sushestvovanie sverhobolochki (supershell) vokrug associacii Skorpiona-Centavra. Solnce voshlo v eto skoplenie mezhzvezdnyh oblakov uzhe posle ego obrazovaniya.


Shema Solnechnoi okrestnosti po Frichu


Vypusk 76. 19-30 aprelya 2004

obzor astro-ph/0404451 Mezhzvezdnaya turbulentnost': nablyudeniya i processy (Interstellar Turbulence I: Observations and Processes)
Authors: Bruce G. Elmegreen, John Scalo
Comments: 72 pages + 5 separate figures, submitted to Annual Reviews of Astronomy and Astrophysics

obzor astro-ph/0404452 Mezhzvezdnaya turbulentnost'. II.: prilozheniya i effekty (Interstellar Turbulence I: Observations and Processes)
Authors: John Scalo, Bruce G. Elmegreen
Comments: 46 pages + 2 separate figures, submitted to Annual Reviews of Astronomy and Astrophysics

Obzor v dvuh chastyah po mezhzvezdnoi turbulentnosti.

Avtory podrobneishim obrazov razbirayut vse bazovyi problemy, svyazannye s turbulentnost'yu, vklyuchaya neplohoi obzor osnovnyh ponyatii (t.e. teorii). Konechno zhe privoditsya mnogo dannyh nablyudenii i podrobnaya bibliografiya. Pozhalui imenno etim obzor i cenen: izlozhenie osnov + bibliografiya.


Vypusk 74. 01-11 aprelya 2004

astro-ph/0404012 Tumannost' MakNeila v Orione: istoriya aktivnosti (Mc Neil's Nebula in Orion: The Outburst History)
Authors: C.Briceno et al.
Comments: 13 pages, 4 figures, accepted to ApJ Letters

Tumannost' MakNeila yavilas' ochen' interesnym otkrytiem zimy etogo goda. Deistvitel'no, lyubitel' astronomii pryamo ryadom s superizvestnoi Tumannost'yu Oriona otkryl novyi ob'ekt! Eshe v sentyabre 2003 g. nikakoi tumannosti tam ne bylo, i vot ....

V stat'e avtory predstavlyayut rezul'taty nablyudenii tumannosti na metrovom shmidtovskom teleskope v Venesuele. Ryad dannyh ohvatyvaet 5-letnii period. Nachalo vspyshki avtory datiruyut mezhdu 28 oktyabrya i 15 noyabrya 2003 g. Obsuzhdaetsya vozmozhnost' togo, chto v sluchae etoi tumannosti my imeem delo s fuorom (istochnikom tipa FU Ori).


Vypusk 68. 01-07 fevralya 2004

miniobzor astro-ph/0402019 Molekulyarnye oblaka v centre Galaktiki (Galactic Center Molecular Clouds)
Authors: R. Guesten, S. Philipp
Comments: 10 pages, 3 figures. Version with full graphics available from ftp://ftp.mpifr-bonn.mpg.de/outgoing/sphilipp (Co)authored by members of the MPIfR (Sub)millimeter Astronomy Group. To appear in the Proceedings of the 4th Cologne-Bonn-Zermatt-Symposium "The Dense Interstellar Medium in Galaxies" eds. S. Pfalzner, C. Kramer, C. Straubmeier, & A. Heithausen (Springer: Berlin)

Yadra aktivnyh (i ne ochen' aktivnyh) galaktik i ih okrestnosti - eto burnyi kotel. Razumeetsya, central'naya chast' nashei Galaktiki yavlyaetsya samym blizkim primerom takih oblastei. Poetomu ee issledovanie predstavlyaet dopolnitel'nyi interes, t.k. my mozhem uznat' koe-chto o processah, kotorye ne mozhem rassmotret' v dalekih galakticheskih yadrah.

V etom obzore rasskazyvaetsya o central'nom molekulyarnom diske (sloe) razmerom primerno 450 na 50 pk. Ego massa sostavlyaet okolo 108 solnechnyh mass. Opisyvaetsya, kak eti molekulyarnye oblaka svyazany so zvezdoobrazovaniem v galakticheskom centre.

Avtory upominayut filamenty (volokna) v centre Galaktiki. Bolee detal'no ob etih obrazoavniyah mozhno prochest' v rabote New Nonthermal Filaments at the Galactic Center: Are They Tracing a Globally Ordered Magnetic Field?.


Vypusk 66. 19-26 yanvarya 2004

obzor astro-ph/0401344 Mezhzvezdnoe pogloshenie v nashei Galaktike (Interstellar Extinction in the Milky Way Galaxy)
Authors: Edward L. Fitzpatrick
Comments: Invited review at the Astrophysics of Dust 2003 Symposium held in Estes Park, Colorado, USA in May 26-30, 2003. Conference proceedings to be published through the ASP Conference Series in 2004, edited by A. Witt, B. Draine, and G. Clayton. 24 pages, including 14 figures

Chitateli navernyaka pomnyat, chto pervye popytki ustanovit' formu i razmer nashei Galaktiki privodili k strannym rezul'tatam: Solnce okazyvalos' vblizi centra. Delo otchasti bylo v tom, chto togda ne znali o mezhzvezdnom pogloshenii sveta. Esli vy ne hotite ostavat'sya v polozhenii uchenyh 18 veka, to chitaite etot obzor. Tam pro pogloshenie sveta (ot IK do UF) podrobno rasskazano.


miniobzor astro-ph/0401428 Mertv li Mestnyi puzyr'? (Is the Local Bubble dead?)
Authors: Dieter Breitschwerdt, Donald P. Cox
Comments: 11 pages, 4 figures, Summary of the Panel Discussion "The Local Bubble", to appear in: Proceedings of the Conference "How the Galaxy Works - Galactic Tertulia: A Tribute to Don Cox and Ron Reynolds'', Granada (Spain), 23-27 June 2003, Kluwer (in press), eds. E.J Alfaro, E. Perez, J. Franco

My uzhe pisali o Mestnom puzyre. Eto svoego roda polost' nepravil'noi formy vnutri kotoroi my i nahodimsya. Polagayut, chto prichinoi obrazovaniya Puzyrya stalo neskol'ko vzryvov sverhnovyh, proizoshedshih na protyazhenii neskol'kih millionov let. S Puzyrem i vzryvami svyazyvayut neskol'ko interesnvyh fenomenov: ot osobennostei v spektre kosmicheskih luchei do ischeznoveniya vidov na Zemle.

V stat'e daetsya kratkii ocherk poslednih issledovanii Mestnogo puzyrya. V osnovnom opisyvayutsya dannye nablyudenii (v tom chisle v ih istoricheskom razvitii). Nekotoroe mesto otvedeno i modelyam (starym i novym).


Vypusk 64. 01-11 yanvarya 2004

astro-ph/0401056 Kol'ca v galo planetarnyh tumannostei (Rings in the Haloes of Planetary Nebulae)
Authors: R.L.M. Corradi et al
Comments: 10 pp., 4 figs, accepted by A&A main journal

Avtory dannoi raboty predprinyali poisk kol'cevyh (i dugoobraznyh) struktur v planetarnyh tumannostyah. I nashli ih! U vos'mi ob'ektov. Teper' takih tumannostei stalo vtroe bol'she. Nalichie takih struktur ukazyvaet, chto peremennost' zvezdnogo vetra v planetarnyh tumannostyah na vremennyh shkalah ot 100 do 1000 let, gorazdo bolee chastoe yavlenie dlya zvezd vblizi konca asimptoticheskoi vetvi gigantov (na diagramma Gercshprunga-Rassela), chem polagalos' ranee. Chislo takih sistem dolzhno sostavlyat' primerno 35%.


Negativnye izobrazheniya chetyreh iz vos'mi tumannostei, u kotoryh naideny kol'cevye struktury. Sleva - ishodnye negativy, v centre i sprava izobrazheniya, povergnutye special'noi obrabotke, na kotoryh horosho vidny kol'ca.


(Arhiv Mezhzvezdnaya sreda:
v.2, 2003, v.1, 2002-2003)

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