Hydrodynamic models of line-driven accretion disk winds in cataclysmic variables

Details Hydrodynamic models of line-driven accretion disk winds in cataclysmic variables Hydrodynamic models of line-driven accretion disk winds in cataclysmic variables

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aipc..431..471p&link_type=abstract

Accretion processes in astrophysical systems: Some like it hot! - eigth astrophysics conference. AIP Conference Proceedings, Vo

Astronomy and Astrophysics

Astrophysics

Accretion And Accretion Disks, Cataclysmic Binaries, Symbiotic Stars, Hydrodynamics

Scientific paper

We present one-dimensional isothermal analytic hydrodynamic models, both one-dimensional and two-dimensional isothermal numerical models, and two-dimensional adiabatic alpha disk numerical models for line-driven accretion disk winds from CVs. Using the one-dimensional analytic models we explore the physical conditions necessary for the existence of a disk wind. Using the two-dimensional isothermal model we explore the effects of centrifugal forces in the wind, and show that these forces cause the wind stream lines to collide producing enhanced density regions in the disk wind. For disk luminosity Ldisk=Lsolar, white dwarf mass Mwd=0.6Msolar, and white dwarf radii Rwd=0.01Rsolar, through the two-dimensional adiabatic alpha disk model we obtain a wind mass-loss rate of 8×10-12Msolar yr-1, a terminal velocity of ~3000 km s-1, and line profiles for CIV (1550 Å) for various angles. The line profiles obtained are consistent with observations in their general form and strong dependence in inclination angle. Thus we are able to predict the general observed wind properties of CVs.

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