Hydrodynamic Models of Line-Driven Accretion Disk Winds in Cataclysmic Varia bles

Details Hydrodynamic Models of Line-Driven Accretion Disk Winds in Cataclysmic Varia bles Hydrodynamic Models of Line-Driven Accretion Disk Winds in Cataclysmic Varia bles

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001rmxac..11..159p&link_type=abstract

"IX Latin American Regional IAU Meeting, "Focal Points in Latin American Astronomy", held in Tonantzintla, Mexico, Nov 9-13, 199

Astronomy and Astrophysics

Astronomy

Scientific paper

We developed several alpha-disk models for line-driven winds from cataclysmi c variables. Using 1-D analytic models we explore the conditions necessary for th e existence of a wind, and the dependence of speed and mass-loss with radius. Using a 2-D isothermal model we explore the effects of centrifugal forces, showing that they cause stream lines to collide producing enhanced density regions in the wind. Without these effects, the mass-loss rates obtained would be too low to produce the optical depths required to explain P-Cygni profiles, showing the necessity of 2-D models. Using a 2-D adiabatic model we calculate mass-losses, terminal velocities, and C IV line profiles for various angles. For a disk with Lsun around a white dwarf of 0.6 Msun and 0.01 Rsun, we obtain dot Mwind=8 × 10-12 Msun yr-1, and a terminal velocity ~ 3000 km s-1. The profiles obtained are consistent with observations, in particular with the absorption of the blue-shifted component, the velocities implied by absorption components, the width of emission components, and the strong dependence with inclination.

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