appall
发表于 2025-3-30 08:49:46
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
FOVEA
发表于 2025-3-30 13:16:54
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悠然
发表于 2025-3-30 19:38:54
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
obstinate
发表于 2025-3-30 22:05:36
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翅膀拍动
发表于 2025-3-31 04:54:08
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妨碍议事
发表于 2025-3-31 07:33:05
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
沙发
发表于 2025-3-31 12:23:41
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
Resection
发表于 2025-3-31 14:22:04
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
Commemorate
发表于 2025-3-31 20:28:42
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
FATAL
发表于 2025-3-31 22:04:48
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