A far ultraviolet archival study of cataclysmic variables. I. FUSE and HST STIS spectra of the exposed white dwarf in dwarf nova systems.
GODON P., SION E.M., BARRETT P.E., HUBENY I., LINNELL A.P. and SZKODY P.
Abstract (from CDS):
We present a synthetic spectral analysis of Far Ultraviolet Spectroscopic Explorer (FUSE) and Hubble Space Telescope Space Telescope Imaging Spectrograph (HST STIS) spectra of five dwarf novae above and below the period gap during quiescence. We use our synthetic spectral code, including options for the treatment of the hydrogen quasi-molecular satellite lines (for low-temperature stellar atmospheres), non-LTE (NLTE) approximation (for high-temperature stellar atmospheres), and for one system (RU Peg) we model the interstellar medium (ISM) molecular and atomic hydrogen lines. In all the systems presented here the FUV flux continuum is due to the white dwarf (WD). These spectra also exhibit some broad emission lines. In this work we confirm some of the previous FUV analysis results, but we also present new results. For four systems we combine the FUSE and STIS spectra to cover a larger wavelength range and to improve the spectral fit. This work is part of our broader HST archival research program, in which we aim to provide accurate system parameters for cataclysmic variables above and below the period gap by combining FUSE and HST FUV spectra.
stars: dwarf novae (SS Aur) - stars: dwarf novae (EY Cyg) - stars: dwarf novae (VW Hyi) - stars: dwarf novae (RU Peg) - stars: dwarf novae (EK TrA) - Stars: White Dwarfs
Table 6 : He 3 not identified, = WD 0644+375