The Evolution of Disks and Winds in Dwarf Novae Outbursts

Details The Evolution of Disks and Winds in Dwarf Novae Outbursts The Evolution of Disks and Winds in Dwarf Novae Outbursts

2001-09-26

arxiv.org/abs/astro-ph/0109486v2

Astronomy and Astrophysics

Astrophysics

10 pages, 3 figures. To appear in "The Physics of Cataclysmic Variables and Related Objects", ASP Conf. Ser., eds. B.T. Gaensi

Scientific paper

Far ultraviolet (FUV) observations are excellent probes of the inner accretion disk, disk outflows, and the mass-accumulating white dwarf in cataclysmic variables. Here we study the contrasting behavior of two canonical dwarf novae in outburst by presenting FUSE FUV (904 -- 1187 A) spectroscopy of U Gem and SS Cyg. We observed each system four times during a single outburst. The outburst peak and early decline spectra of SS Cyg are well fit by models of a steady-state accretion disk and a biconical wind. A broad, blueshifted OVI wind-formed absorption line is the only strong spectral feature. In late outburst decline, OVI and CIII lines are seen as broad emission features and the continuum has flattened. In U Gem, the continua of the optical outburst plateau spectra are plausibly fit by accretion disk model spectra. The spectra also show numerous narrow, low-velocity absorption lines that do not originate in the inner accretion disk. We discuss the line spectra in the context of partial absorption of the FUV continuum by low-velocity, vertically-extended material located at large disk radii. The late outburst decline spectrum of U Gem is dominated by the white dwarf. WD model fits confirm the sub-solar C and super-solar N abundances found in earlier studies.

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