The Rotation, Masses and Chemical Abundances of the White Dwarfs in WZ Sagittae and VW Hydri

Details The Rotation, Masses and Chemical Abundances of the White Dwarfs in WZ Sagittae and VW Hydri The Rotation, Masses and Chemical Abundances of the White Dwarfs in WZ Sagittae and VW Hydri

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6084s&link_type=abstract

HST Proposal ID #6084

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Hst Proposal Id #6084 Hot Stars

Scientific paper

The central accreting object in compact binaries and other accreting systems is usually hidden from direct observation, enshrouded by optically thick accretion disks which are opaque to the radiation emitted by the central object as it accretes matter. In the dwarf novae WZ Sagittae and VW Hydri the underlying white dwarf accreter is clearly exposed in the far UV during quiescence. Orbital phase-resolved GHRS spectra near the quadratures (0.25 and 0.75) of their orbits during quiescence will deliver the following fundamental information: (1) the white dwarf rotation rates, yielding critical information on the boundary layer temperature/structure and spinup of the white dwarfs by accretion; (2) the orbital velocity semi-amplitudes and hence white dwarf masses, independent of disk emission line velocities; (3) delineation by profile shape and velocity,of lower temperature line formation regions associated with the rotating photosphere of the white dwarf from line formation region(s) of higher temperature ion species associated with a boundary layer/accretion belt (or putative hot corona?) still present surrounding the white dwarf; (4) detection of weak metal line profiles and variations versus phase in WZ Sagittae to test accretion versus dredgeup for the origin of carbon, and test physical mechanisms that control the flow of accreted elements and hence abundance changes (diffusion, mixing, dilution, dredeup and ongoing accretion during quiescence).

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