GHRS Spectroscopy of the Exposed White Dwarf in the High Accretion Rate Dwarf Nova RX and

Details GHRS Spectroscopy of the Exposed White Dwarf in the High Accretion Rate Dwarf Nova RX and GHRS Spectroscopy of the Exposed White Dwarf in the High Accretion Rate Dwarf Nova RX and

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6700s&link_type=abstract

HST Proposal ID #6700

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Hst Proposal Id #6700 Binaries And Star Fo

Scientific paper

Out of the six dwarf novae with exposed white dwarfs studiedwith Hubble during quiescence, only one, U Gem, lies above theperiod gap where mass transfer rates are generally higher andwhere the white dwarfs appear to be hotter (younger?) in CVsystems with quite possibly shorter evolutionary histories. RXAnd and its exposed white dwarf fills an absolutely criticalneed for another system above the gap. Orbital Phase-resolvedGHRS G140L observations near the quadratures of its orbitduring quiescence will deliver the following fundamentalinformation: (1) the white dwarf rotation rate; (2) the T_eff, log g and chemical abundances of the white dwarf; (3) theorbital velocity semi-amplitudes and hence a white dwarf massindependent of disk emission line velocities; (4) delineationby profile structure, line formation regions associated with acooler more slowly rotating white dwarf photosphere versusformation regions of higher temperature ion species associatedwith a boundary layer/accretion belt (or putative hot corona?)still present surrounding the white dwarf; (5) the coolingresponse of the white dwarf to compressional and irradiativeheating by the dwarf nova event (does it explain the UV fluxdecline, a problem for disk instability models?); (6) tests ofphysical mechanisms that control the flow of accreted elementsand hence abundance changes (diffusion, mixing/dilutiondredgeup and ongoing accretion during quiescence).

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