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Session 85 - Cataclysmic Variables and Accretion Disks.
Oral session, Wednesday, January 15
Harbour A,
We present the results of hydrodynamic models of the winds from accretion disks in cataclysmic variables. These winds are driven by radiation pressure from the disk continuum acting on the line transitions in the wind material, equivalent to the mechanism which drives strong winds in OB stars. We assume the disk to be a Shakura and Sunyaev \alpha disk and treat the wind adiabatically. We obtain mass loss rates, wind velocity distributions, and calculate theoretical line profiles. We compare the results with our previous one dimensional analytic and numerical models and two dimensional numerical models in which we had assumed an isothermal disk and an isothermal wind. We find that rotational forces are very important in determining the geometry of the winds, a fact which can only be treated accurately in more than one dimension. Theoretical line profiles are found to agree qualitatively with observations.
