Resonance line-profile calculations based on hydrodynamical models of cataclysmic variable winds

Details Resonance line-profile calculations based on hydrodynamical models of cataclysmic variable winds Resonance line-profile calculations based on hydrodynamical models of cataclysmic variable winds

2002-02-21

arxiv.org/abs/astro-ph/0202384v1

Astronomy and Astrophysics

Astrophysics

LaTeX, 19 pages, to appear in ApJ

Scientific paper

10.1086/340339

We present synthetic line profiles as predicted by the models of 2-D line- driven disk winds due to Proga, Stone & Drew. We compare the model line profiles with HST observations of the cataclysmic variable IX Vel. The model wind consists of a slow outflow that is bounded on the polar side by a fast stream. We find that these two components of the wind produce distinct spectral features. The fast stream produces profiles which show features consistent with observations. These include the appearance of the P-Cygni shape for a range of inclinations, the location of the maximum depth of the absorption component at velocities less than the terminal velocity, and the transition from absorption to emission with increasing inclination. However the model profiles have too little absorption or emission equivalent width. This quantitative difference between our models and observations is not a surprise because the line-driven wind models predict a mass loss rate that is lower than the rate required by the observations. We note that the model profiles exhibit a double-humped structure near the line center which is not echoed in observations. We identify this structure with a non-negligible redshifted absorption which is formed in the slow component of the wind where the rotational velocity dominates over expansion velocity. We conclude that the next generation of disk wind models, developed for application to CVs, needs to yield stronger wind driving out to larger disk radii than do the present models.

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