標(biāo)題: Titlebook: Cataclysmic Variables and Related Objects; Proceedings of the 7 Mario Livio,Giora Shaviv Conference proceedings 1983 D. Reidel Publishing C [打印本頁] 作者: 小天使 時(shí)間: 2025-3-21 17:09
書目名稱Cataclysmic Variables and Related Objects影響因子(影響力)
書目名稱Cataclysmic Variables and Related Objects影響因子(影響力)學(xué)科排名
書目名稱Cataclysmic Variables and Related Objects網(wǎng)絡(luò)公開度
書目名稱Cataclysmic Variables and Related Objects網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Cataclysmic Variables and Related Objects被引頻次
書目名稱Cataclysmic Variables and Related Objects被引頻次學(xué)科排名
書目名稱Cataclysmic Variables and Related Objects年度引用
書目名稱Cataclysmic Variables and Related Objects年度引用學(xué)科排名
書目名稱Cataclysmic Variables and Related Objects讀者反饋
書目名稱Cataclysmic Variables and Related Objects讀者反饋學(xué)科排名
作者: 拍翅 時(shí)間: 2025-3-21 21:59
One Hundred Years of Social ProtectionWe present results of recent spectroscopic observations of A) some LMC X-ray sources, B) the X-ray burster 1735-44, and C) the peculiar emission-line binary BE UMa. From the short time scale variations and inferred low mass components each shows some similarities to more classical CV’s.作者: decipher 時(shí)間: 2025-3-22 02:15 作者: 白楊 時(shí)間: 2025-3-22 05:30 作者: Magnitude 時(shí)間: 2025-3-22 10:48 作者: 招待 時(shí)間: 2025-3-22 15:58 作者: 招待 時(shí)間: 2025-3-22 21:08
Did Nova Aquilae 1982 Possess a Supercritical Wind ?,The extremely high velocity absorption components observed in the ultraviolet with IUE, could have been produced by a supercritical wind. In this case most radiation would have been emitted shortwards of Lyman α, even at the time of the first IUE observations.作者: 支形吊燈 時(shí)間: 2025-3-22 23:08 作者: 顯赫的人 時(shí)間: 2025-3-23 04:51
Infrared Spectra of Nova Dust Shells,Results of fitting blackbody and pseudoblackbody functions to infrared photometry for three classical novae are briefly summarised.作者: Brocas-Area 時(shí)間: 2025-3-23 09:33
https://doi.org/10.1007/978-3-030-54606-9, and other physical properties. Unfortunately, despite an abundance of observational data on these systems, there is a severe dearth of reliable, quantitative information about their fundamental physical properties. Only two cataclysmic variables, U Gem and EM Cyg, are simultaneously eclipsing bina作者: 燈泡 時(shí)間: 2025-3-23 13:19
One Hundred Years of Social Protectionher studied in detail on the bases of UBV- colours, multi-channel photoelectric light curves and image-tube spectrograms which were newly obtained at Tokyo Astronomical Observatory. The result of analysis of these materials for the nature of the cataclysmic variable is presented.作者: 危險(xiǎn) 時(shí)間: 2025-3-23 14:47
One Hundred Years of Social Protectionn 0 or WR star and a black hole surrounded by a luminous precessing accretion disk (from which emanate spectacular relativistic jets); the second, GK Per, is a classical old nova consisting of a slightly evolved K2 star and an unseen white dwarf companion surrounded by an accretion disk which is les作者: 恫嚇 時(shí)間: 2025-3-23 19:28
One Hundred Years of Social Protectionnd that WZ Sge was an eclipsing binary with an 81 min 38 s orbital period. Krzeminski and Kraft (1964, hereafter KK) in the first of many comprehensive analyses of the WZ Sge system to appear in the literature stated “a lower limit to certain detection of orbital velocity changes for the double emis作者: 緯度 時(shí)間: 2025-3-23 22:25
https://doi.org/10.1007/978-3-030-54959-6ary analysis of the data shows that the line emitting gas is probably photoionized by a hot, T. ? 200,000 ?K continuum, which can explain the extremely strong Hell lines. The hydrogen Balmer line intensities are different from what is predicted by recombination theory and the optical depths in Hα an作者: Lucubrate 時(shí)間: 2025-3-24 03:57 作者: OMIT 時(shí)間: 2025-3-24 06:39
One Hundred Years of Social Protectionthe time-dependent evolution of viscous accretion discs. These models are axisymmetric, with the vertical structure reduced to integrated averages of local physical conditions. Published work examines models of dwarf nova eruptions driven by mass transfer bursts (Bath & Pringle 1981 — Paper I), erup作者: 苦澀 時(shí)間: 2025-3-24 14:30
One Hundred Years of Social Protectionresponsible for the hump, or shoulder, that occurs. prior to eclipse in the quiescent state, and, in systems with suitable inclination such as II Gem, responsible also for the primary eclipse itself. In systems with higher inclination such as Z Cha, the primary eclipse is composed of both this aniso作者: META 時(shí)間: 2025-3-24 17:50 作者: Infusion 時(shí)間: 2025-3-24 21:30 作者: 背書 時(shí)間: 2025-3-25 02:53 作者: Delude 時(shí)間: 2025-3-25 07:14 作者: Graduated 時(shí)間: 2025-3-25 09:11 作者: ARC 時(shí)間: 2025-3-25 12:19 作者: enterprise 時(shí)間: 2025-3-25 16:33
Cataclysmic Variables and Related Objects978-94-009-7118-9Series ISSN 0067-0057 Series E-ISSN 2214-7985 作者: CULP 時(shí)間: 2025-3-25 21:14 作者: Congestion 時(shí)間: 2025-3-26 03:35 作者: 胰島素 時(shí)間: 2025-3-26 05:44 作者: 散開 時(shí)間: 2025-3-26 10:11 作者: 我沒有強(qiáng)迫 時(shí)間: 2025-3-26 13:03
Photometric and Spectroscopic Observations of the Cataclysmic Variable AC Cancri,her studied in detail on the bases of UBV- colours, multi-channel photoelectric light curves and image-tube spectrograms which were newly obtained at Tokyo Astronomical Observatory. The result of analysis of these materials for the nature of the cataclysmic variable is presented.作者: 承認(rèn) 時(shí)間: 2025-3-26 18:19
Recent Spectroscopy of X-Ray Sources and Systems Related to Cataclysmic Variables: II,n 0 or WR star and a black hole surrounded by a luminous precessing accretion disk (from which emanate spectacular relativistic jets); the second, GK Per, is a classical old nova consisting of a slightly evolved K2 star and an unseen white dwarf companion surrounded by an accretion disk which is less luminous than the K2 star.作者: 轉(zhuǎn)換 時(shí)間: 2025-3-26 22:49 作者: 輕率的你 時(shí)間: 2025-3-27 02:30 作者: Armory 時(shí)間: 2025-3-27 09:19 作者: 優(yōu)雅 時(shí)間: 2025-3-27 10:16 作者: 堅(jiān)毅 時(shí)間: 2025-3-27 16:02 作者: prostatitis 時(shí)間: 2025-3-27 20:38
CNO Abundances and Nova Outburst Strengths,, deduced from the accretion disk luminosity, is too high to permit a strong enough hydrogen flash to give the observed nova strength. Some possible resolutions to this paradox are suggested..Recurrent novae are probably not themonuclear runaways on accreting white dwarfs.作者: callous 時(shí)間: 2025-3-28 01:43
The Formation of Optical CNO Emission Lines in Cataclysmic Variables,nes of carbon are also present in old novae, probably formed by recombination processes. The available data for the optical CNO lines suggest that non-solar CNO enhancements exist in quiescent novae, indicating that some of the binary systems may be evolved.作者: 讓空氣進(jìn)入 時(shí)間: 2025-3-28 02:11
Optimal Control Under Stochastic Uncertainty, deduced from the accretion disk luminosity, is too high to permit a strong enough hydrogen flash to give the observed nova strength. Some possible resolutions to this paradox are suggested..Recurrent novae are probably not themonuclear runaways on accreting white dwarfs.作者: Tracheotomy 時(shí)間: 2025-3-28 10:03
Controlled Random Search Under Uncertaintynes of carbon are also present in old novae, probably formed by recombination processes. The available data for the optical CNO lines suggest that non-solar CNO enhancements exist in quiescent novae, indicating that some of the binary systems may be evolved.作者: ARIA 時(shí)間: 2025-3-28 11:11 作者: Nebulous 時(shí)間: 2025-3-28 17:05
On Evolutionary Models for SNI Progenitor Stars,tionary sequences of an initially cool pure .C 1.0 M. WD show that nearly half of the carbon near the base of the accreted layer, initially of solar composition, gravitationally diffuses out in 2 x 10. years.作者: modish 時(shí)間: 2025-3-28 21:43 作者: 戲服 時(shí)間: 2025-3-29 02:18 作者: 大門在匯總 時(shí)間: 2025-3-29 06:12 作者: Gnrh670 時(shí)間: 2025-3-29 09:25
One Hundred Years of Social Protection responsible also for the primary eclipse itself. In systems with higher inclination such as Z Cha, the primary eclipse is composed of both this anisotropic disc component and the inner-disc/white-dwarf primary component.作者: 預(yù)感 時(shí)間: 2025-3-29 15:22 作者: 有幫助 時(shí)間: 2025-3-29 16:23 作者: 無畏 時(shí)間: 2025-3-29 22:06
Alpha Beta Discs,local physical conditions. Published work examines models of dwarf nova eruptions driven by mass transfer bursts (Bath & Pringle 1981 — Paper I), eruptions produced by global viscous changes within the disc (Bath & Pringle 1982a — Paper II), and the time-dependent properties of giant discs in symbiotic binaries (Bath & Pringle 1982b - Paper III).作者: Annotate 時(shí)間: 2025-3-30 01:05 作者: 礦石 時(shí)間: 2025-3-30 04:41 作者: appall 時(shí)間: 2025-3-30 08:49
The Periods of Cataclysmic Variable Stars,, and other physical properties. Unfortunately, despite an abundance of observational data on these systems, there is a severe dearth of reliable, quantitative information about their fundamental physical properties. Only two cataclysmic variables, U Gem and EM Cyg, are simultaneously eclipsing bina作者: FOVEA 時(shí)間: 2025-3-30 13:16 作者: 悠然 時(shí)間: 2025-3-30 19:38
Recent Spectroscopy of X-Ray Sources and Systems Related to Cataclysmic Variables: II,n 0 or WR star and a black hole surrounded by a luminous precessing accretion disk (from which emanate spectacular relativistic jets); the second, GK Per, is a classical old nova consisting of a slightly evolved K2 star and an unseen white dwarf companion surrounded by an accretion disk which is les作者: obstinate 時(shí)間: 2025-3-30 22:05 作者: 翅膀拍動(dòng) 時(shí)間: 2025-3-31 04:54 作者: 妨礙議事 時(shí)間: 2025-3-31 07:33
KQ Mon and the Nature of the UX Ursa Majoris Nova-Like Variables,y similar to other members of the UX Ursa Majoris subset. However its ultraviolet spectra when compared with other UX UMa stars shed considerable light on the nature of these objects. Its spectrum is dominated by strong broad highly ionized absorption lines including the NV, Si IV and CIV UV resonan作者: 沙發(fā) 時(shí)間: 2025-3-31 12:23
Alpha Beta Discs,the time-dependent evolution of viscous accretion discs. These models are axisymmetric, with the vertical structure reduced to integrated averages of local physical conditions. Published work examines models of dwarf nova eruptions driven by mass transfer bursts (Bath & Pringle 1981 — Paper I), erup作者: Resection 時(shí)間: 2025-3-31 14:22
Humps and Superhumps,responsible for the hump, or shoulder, that occurs. prior to eclipse in the quiescent state, and, in systems with suitable inclination such as II Gem, responsible also for the primary eclipse itself. In systems with higher inclination such as Z Cha, the primary eclipse is composed of both this aniso作者: Commemorate 時(shí)間: 2025-3-31 20:28
CNO Abundances and Nova Outburst Strengths,hancement of CNO abundances, relative to the Sun, is necessary for fast novae yet slow novae, such as DQ Her, can still occur with large CNO abundances. An analysis of observational data indicates that the white dwarfs in nova binaries have masses typically 1.1 For some old novae, the accretion rate作者: FATAL 時(shí)間: 2025-3-31 22:04 作者: Congeal 時(shí)間: 2025-4-1 05:25
The Continuum Energy Distribution of the Old-Nova GK PER (1901),extinction,is found to be consistent with the model of an accreting magnetic white dwarf. Furthermore, we discuss plausible modifications of the standard disc structure caused by the presence of magnetic field lines threading the disc and evaluate the contribution to the observed radiation field fro作者: debacle 時(shí)間: 2025-4-1 09:31 作者: 厚臉皮 時(shí)間: 2025-4-1 10:59 作者: NOVA 時(shí)間: 2025-4-1 17:17
Physical Conditions Inside White Dwarfs and Type I Supernovae, the problem was not studied until Schatzman (19 74) described the competition between collapse dominated by beta decay, which would lead to neutron star formation and collapse dominated by nuclear reactions leading to stellar disruption.作者: buoyant 時(shí)間: 2025-4-1 22:10 作者: Biguanides 時(shí)間: 2025-4-1 23:09
