The UV Spectrum of an Elliptical Accretion Disk Devoid of Hydrogen

Details The UV Spectrum of an Elliptical Accretion Disk Devoid of Hydrogen The UV Spectrum of an Elliptical Accretion Disk Devoid of Hydrogen

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8159w&link_type=abstract

HST Proposal ID #8159

Computer Science

Hst Proposal Id #8159 Binary Stars

Scientific paper

AM CVn {HZ 29} is the prototype of the interacting double- degenerate binaries, or so-called Helium Cataclysmic Variables {He CVs}, which could be a channel to form Type Ia supernovae. These are short-orbital period systems in which a low-mass He white dwarf orbits a more massive white dwarf and transfers matter devoid of hydrogen to an accretion disk around that star. AM CVn is the best He CV to measure the mass transfer rate {dM/dt} and the chemical abundance pattern of the transferred material. Lines from different ions of the same element arise at different radii in the disk, and have different velocity widths. This makes a mapping of temperature onto radius possible, and with it a determination of dM/dt. This modeling is best done using ultraviolet spectra, where the necessary lines can be found. Observations by HST/STIS are needed, to provide the combination of high spectral and temporal resolution and signal-to-noise ratio, and wide spectral coverage that neither IUE nor prior HST/GHRS spectra provide. The data can be used in a variety of ways. We will undertake a modeling study of the steady-state spectrum of AM CVn. We will learn whether only H-burning took place in the mass donor or whether 3Alpha He-burning also occurred. Comparing H-rich and H-depleted disks will also tell us about the stability of disks and their ability to drive winds.

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