Titlebook: Cataclysmic Variables and Related Objects; Proceedings of the 7 Mario Livio,Giora Shaviv Conference proceedings 1983 D. Reidel Publishing C

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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

悠然

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

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妨碍议事

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

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

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

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