Results 21 to 30 of about 2,620,915 (156)
The component masses of the cataclysmic variable V347 Puppis [PDF]
, 2005 We present time-resolved spectroscopy and photometry of the double-lined eclipsing cataclysmic variable V347 Pup (=LB 1800). There is evidence of irradiation on the inner hemisphere of the secondary star, which we correct for using a model to give a ...
Buckley, D. A. H. +17 more
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K-band spectroscopy of pre-cataclysmic variables [PDF]
, 2007 Aims. There exists now substantial evidence for abundance anomalies in a number of cataclysmic variables (CVs), indicating that the photosphere of the secondary star incorporates thermonuclear processed material. However, the spectral energy distribution
Navarrete, F. P. +9 more
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THE EVOLUTION OF CATACLYSMIC VARIABLES AS REVEALED BY THEIR DONOR STARS [PDF]
The Astrophysical Journal Supplement Series, 2011 ABSTRACT We present an attempt to reconstruct the complete evolutionary path followed by cataclysmic variables (CVs), based on the observed mass–radius relationship of their donor stars. Along the way, we update the semi-empirical CV donor sequence presented previously by one of
Knigge, Christian +2 more
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Cataclysmic Variable Stars [PDF]
Highlights of Astronomy, 1998 The evolution of single stars on and away from the main sequence is well understood. A degenerate core is formed in a star as the star leaves the main sequence and expands to a giant with a radius typically 50 - 500 Ro . Observationally it is known that most stars are members of binary systems, and among these many have orbital periods less than 100 y.
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Mass Determinations of Cataclysmic Variables [PDF]
, 2013 Cataclysmic variables (CVs) are a class of closely interacting binary system that undergo mass transfer from a Roche lobe filling secondary star to a white dwarf primary star, usually via a gas stream and an accretion disc.
Savoury, C.D.J.
core +5 more sources
Cataclysmic Variables as Binary Stars: Then and Now [PDF]
International Astronomical Union Colloquium, 1990 AbstractA brief history is given of the clues that led to the establishment, in the period c. 1950 to 1965, of a universal binary model for novae and related cataclysmic variables. The observational facts, established early in this period by A. H. Joy and R. F. Sanford (selected binary orbits), J. L. Greenstein (spectroscopy) and M. Walker (photometry)
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Indirect Imaging of Cataclysmic Variable Stars [PDF]
, 2022 Kataklysmische veränderliche Sterne (CVs) sind kompakte Doppelsterne, die aus einem weißen Zwerg, einem späten Hauptreihenstern und einer Akkretionsstruktur bestehen. Die scheinbare Ausdehnung der Objekte ist wegen der großen Entfernung zu klein, um direkte räumlich aufgelöste Abbildungen aufzunehmen.
Kube, Jens +4 more
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, 2023 Cataclysmic variable stars are semi-detached binary systems consisting of a white dwarf primary star and a late-type secondary star. The secondary star in these systems is over- filling its Roche lobe, which enables a mass transfer to occur between the ...
Kára, Jan
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The Astronomical Journal, 2023 Accretion of mass onto a white dwarf (WD) in a binary system can lead to stellar explosions. If a WD accretes from stellar wind of a distant evolved giant in a symbiotic binary, it can undergo occasional outbursts in which it brightens by several ...
Augustin Skopal
doaj +1 more source
The Periods of Cataclysmic Variable Stars [PDF]
International Astronomical Union Colloquium, 1983 To understand the structure and evolution of the cataclysmic variables, we will need accurate values for their masses, dimensions, mass transfer rates, 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
openaire +1 more source