The Accretion Rate and Temperature of the Accreting White dwarf in the Dwarf Nova SS Cygni During Quiescence

Details The Accretion Rate and Temperature of the Accreting White dwarf in the Dwarf Nova SS Cygni During Quiescence The Accretion Rate and Temperature of the Accreting White dwarf in the Dwarf Nova SS Cygni During Quiescence

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.4412l&link_type=abstract

American Astronomical Society Meeting 203, #44.12; Bulletin of the American Astronomical Society, Vol. 35, p.1276

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Using the the newly determined parallax for the dwarf nova SS Cygni, we have analyzed IUE archival spectra of the system during quiescence. The spectra are fit poorly by optically thick accretion disk models alone. The best-fitting composite white dwarf plus accretion disk models to the most representative quiescent spectra yield Teff = 35,000K ± 1000K, ˙ {M} = 5× 10-11 M&sun;/yr, i = 41o, with a scale factor-derived distance of 166 pc, in excellent agreement with the distance of 166 pc from the trigonometric parallax. During quiescence, the accretion disk dominates the FUV flux. In contrast with quiescence, a best-fitting steady state disk model to a typical outburst spectrum yielded an accretion rate of 4× 10-9 M&sun;/yr and a scale factor-derived distance of 162 pc, in close agreement with the parallax distance. During outburst the accretion disk provides essentially all of the FUV flux.
This work was supported by NASA grant NAG5-11182 to Villanova University and by a summer undergraduate research grant from the Delaware Space Grant Consortium.

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