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- Q1059564 subject Q5894358.
- Q1059564 subject Q7061010.
- Q1059564 subject Q8346772.
- Q1059564 subject Q8728797.
- Q1059564 abstract "Cataclysmic variable stars (CV) are stars which irregularly increase in brightness by a large factor, then drop back down to a quiescent state. They were initially called novae, from the Latin 'new', since ones with an outburst brightness visible to the naked eye and an invisible quiescent brightness appeared as new stars in the sky.Cataclysmic variable stars are binary stars that consist of two components; a white dwarf primary, and a mass transferring secondary. The stars are so close to each other that the gravity of the white dwarf distorts the secondary, and the white dwarf accretes matter from the companion. Therefore, the secondary is often referred to as the donor star. The infalling matter, which is usually rich in hydrogen, forms in most cases an accretion disc around the white dwarf. Strong UV and X-ray emission is often seen from the accretion disc. The accretion disk may be prone to an instability leading to dwarf nova outbursts, when a portion of the disk material falls onto the white dwarf, resulting in release of radiation derived from the loss of gravitational potential energy. The brighter and less frequent nova outbursts occur when the density and temperature at the bottom of the accumulated hydrogen layer rise high enough to ignite runaway hydrogen fusion reactions, which rapidly convert the hydrogen layer to helium.If the accretion process continues long enough to bring the white dwarf close to the Chandrasekhar limit, the increasing interior density may ignite runaway carbon fusion and trigger a Type Ia supernova explosion, which would completely destroy the white dwarf.".
- Q1059564 thumbnail Accretion_Disk_Binary_System.jpg?width=300.
- Q1059564 wikiPageExternalLink index.html.
- Q1059564 wikiPageExternalLink cvstext.html.
- Q1059564 wikiPageExternalLink www.cvcat.net.
- Q1059564 wikiPageExternalLink RKcat.
- Q1059564 wikiPageExternalLink cv_beginners.html.
- Q1059564 wikiPageExternalLink aavsocvsection.
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- Q1059564 wikiPageWikiLink Q5894358.
- Q1059564 wikiPageWikiLink Q6458.
- Q1059564 wikiPageWikiLink Q7061010.
- Q1059564 wikiPageWikiLink Q8346772.
- Q1059564 wikiPageWikiLink Q8728797.
- Q1059564 wikiPageWikiLink Q908282.
- Q1059564 wikiPageWikiLink Q909534.
- Q1059564 comment "Cataclysmic variable stars (CV) are stars which irregularly increase in brightness by a large factor, then drop back down to a quiescent state. They were initially called novae, from the Latin 'new', since ones with an outburst brightness visible to the naked eye and an invisible quiescent brightness appeared as new stars in the sky.Cataclysmic variable stars are binary stars that consist of two components; a white dwarf primary, and a mass transferring secondary.".
- Q1059564 label "Cataclysmic variable star".
- Q1059564 depiction Accretion_Disk_Binary_System.jpg.