The Hot Components of AM CVn Helium Cataclysmics

Details The Hot Components of AM CVn Helium Cataclysmics The Hot Components of AM CVn Helium Cataclysmics

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21733805s&link_type=abstract

American Astronomical Society, AAS Meeting #217, #338.05; Bulletin of the American Astronomical Society, Vol. 43, 2011

Physics

Scientific paper

The AM CVn helium-transfer cataclysmic variables are fundametally important because they are the progeny of double common envelope evolution, they are a principal source of low frequency gravitational wave emission, a laboratory for accretion and interior physics under extreme conditions and candidates for Type Ia supernovae. The hot component, consisting of a helium-rich white dwarf and disk, is the focus of our synthetic spectral analysis using the code BINSYN (Linnell& Hubeny 1996) which takes into account the donor companion star, the shock front which forms at the disk edge and the FUV and NUV energy distribution.
We report the first results from our multi-component study of helium accretion and white dwarf heating.
This research was supported by NASA ADP grant NN09AC94G and in part by NSF grant AST0807892, both to Villanova University.

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