Computer Science
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5362r&link_type=abstract
HST Proposal ID #5362
Computer Science
Hst Proposal Id #5362 Hot Stars Eruptive Binaries
Scientific paper
We propose to exploit the unique UV capabilities of the HST FOS to obtain the first time-resolved, high-resolution UV spectroscopy of the wind outflow in the enigmatic cataclysmic binary, V795 Her. Our previous IUE observations of this star have revealed extraordinary UV properties. Specifically, the SiIV and CIV line profiles change markedly on timescales at least as fast as the 30 minute exposure limit imposed by the sensitivity of IUE. Moreover, repeat observations over several allocation rounds have confirmed a coherent modulation on a period of 4.86hrs rather than at the known optical periods. It is well-established that many disk-accreting CVs show periodic UV line profile variation, but V795 Her breaks the mould in varying on a period that appears not to be the orbital period. A plausible origin for the usual orbital variation is wind shadowing of asymmetric disk structure induced by the mass transfer stream. However, it remains to be established whether such a model can be applied to the peculiar case of V795 Her. Indeed, it is unlikely that the intrinsic wind properties hold the key to the periodic UV line behaviour since the natural timescale of the wind source, believed to be seated in the inner disk, is of order minutes. The primary objectives are 1) to investigate and quantify radial velocity motion in the CIV emission component, 2) to define the nature and shortest timescales of variation in both the SiIV and CIV line profiles, 3) to measure any correlated continuum flux changes.
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