Modeling The Hot Components In Cataclysmic Variables: Info On The White Dwarf And Hot Disk From GALEX, FUSE, HST And SDSS

Details Modeling The Hot Components In Cataclysmic Variables: Info On The White Dwarf And Hot Disk From GALEX, FUSE, HST And SDSS Modeling The Hot Components In Cataclysmic Variables: Info On The White Dwarf And Hot Disk From GALEX, FUSE, HST And SDSS

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.3801s&link_type=abstract

American Astronomical Society Meeting 208, #38.01; Bulletin of the American Astronomical Society, Vol. 38, p.113

Astronomy and Astrophysics

Astronomy

Scientific paper

The active accretion from the late type dwarf secondary star to the white dwarf in the close binary systems known as cataclysmic variables results in heating effects throughout these systems. These effects can be explored by modeling the observed UV through optical light curves obtained for these objects during different states of accretion, as well as by fitting the individual spectral lines and combined spectral energy distributions. Recent results using data from GALEX, FUSE, HST and the SDSS have advanced our understanding in several ways. They have enabled us to determine the hottest and coolest white dwarfs present in accreting systems. The temperatures of pulsating white dwarfs in cataclysmic variables as compared to single ZZ Ceti stars is emerging. It has become apparent that even when optical observations indicate the accretion has turned off in systems containing highly magnetic white dwarfs, the UV still shows some hot regions on the white dwarf. At high accretion rates, there are many complexities involved in separating the white dwarf from the accretion disk and in obtaining a correct model for the disk that matches the fluxes observed over a large wavelength range and the emission lines. Thus, our understanding of heating effects is still a work in progress.This work was supported by NASA grants for GALEX, FUSE and HST and an NSF grant for SDSS.

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