The nature of the bright 'Supersoft X-ray Source' RX J 0019+21

Details The nature of the bright 'Supersoft X-ray Source' RX J 0019+21 The nature of the bright 'Supersoft X-ray Source' RX J 0019+21

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7346b&link_type=abstract

HST Proposal ID #7346

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Hst Proposal Id #7346 Binary Stars

Scientific paper

RX J0019+21 is by far the brightest member of the new still small class of close-binary `Supersoft X-ray Sources' which probably contain a near-Eddington accreting and nuclear burning white dwarf. Supersoft X-ray sources radiate most of their energy in the UV and soft X-ray bands with a wealth of information contained in the UV. With V=12, RX J0019+21 is the prime candidate for an in-depth UV study. It may also be the only example of an intermittently burning white dwarf. The STIS is needed to obtain decisive information on the true nature of this unique source. We propose to use the STIS to obtain two sets of echelle spectra of RX J0019+21 at the quadrature phases of the binary orbit. We will be able to determine the UV spectral energy distribution, to separate stellar and interstellar components of e.g. IonCII, IonSiII, IonSiIII and IonOI absorption lines, to search for <~ absorption of stellar or disk origin, measure the profile of the LineHeII1640 emission line, and search for other emission/absorpti on lines. Such information is required to determine the structure and the temperature distribution of the putative accretion disk, to model the wind component, to derive elemental abundances, to obtain an independent estimate of the distance, and to test the combined results against current models for `Supersoft Sources'.

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