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E.M. Sion, F. Cheng, P. Godon (Villanova University), P. Szkody (University of Washington)
We have analyzed the Far Ultraviolet Spectrocopic Explorer (FUSE) spectra of two U Gem-Type dwarf novae, SS Aur and RU Peg. SS Aur was observed 28 days after the last previous dwarf nova outburst and RU Peg was observed 60 days after its last outburst. In both systems the FUSE spectra (905-1182 A) reveal the underlying accreting white dwarf which is clearly exposed in the far UV. Our grid of theoretical models yielded a best-fitting photosphere to the FUSE spectrum of SS Aur with the following parameters: Twd/1000 (K) = 31 + 4/-1, log g = 8.5, Si= 1.0 + 0.2/-0.2 times solar, C = 0.1 + 0.4/-0.1 times solar, N = 2.0 +1.8/-1.5, and Vrot sin i (km/s) = 400 + 100/-70. For RU Peg, our model grid yielded Twd/1000 (K) = 49 + 6/-7, log g (fixed) = 8.5, Si= 0.1 + 0.3/-0.1 times solar, C = 0.1 + 1.7/-0.1 times solar, Vrot sin i = (km/s) = 100 + 500/-100, Scale factor = 6.07396x1.e-04 For SS Aur's white dwarf, the absence of C III (1175) underscores its C-deficiency. Implications are discussed.
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.