Hydrodynamic Models of Line-Driven Accretion Disk Winds II: Adiabatic Winds from Nonisothermal Disks

Details Hydrodynamic Models of Line-Driven Accretion Disk Winds II: Adiabatic Winds from Nonisothermal Disks Hydrodynamic Models of Line-Driven Accretion Disk Winds II: Adiabatic Winds from Nonisothermal Disks

2000-11-03

arxiv.org/abs/astro-ph/0011072v1

The Astrophysical Journal 532 (2000) 563-580

Astronomy and Astrophysics

Astrophysics

67 pages, 28 Postscript figures, uses aasms4.sty and epsf.sty

Scientific paper

10.1086/308527

We present here numerical hydrodynamic simulations of line-driven accretion disk winds in cataclysmic variable systems. We calculate wind mass-loss rate, terminal velocities, and line profiles for CIV (1550 A) for various viewing angles. The models are 2.5-dimensional, include an energy balance condition, and calculate the radiation field as a function of position near an optically thick accretion disk. The model results show that centrifugal forces produce collisions of streamlines in the disk wind which in turn generate an enhanced density region, underlining the necessity of two dimensional calculations where these forces may be represented. For disk luminosity Ldisk = Lsun, white dwarf mass Mwd = 0.6 Msun, and white dwarf radii Rwd = 0.01 Rsun, we obtain a wind mass-loss rate of dMwind/dt = 8.0E-12 Msun/yr, and a terminal velocity of ~3000 km/s. The line profiles we obtain are consistent with observations in their general form, in particular in the maximum absorption at roughly half the terminal velocity for the blue-shifted component, in the magnitudes of the wind velocities implied by the absorption components, in the FWHM of the emission components, and in the strong dependence in inclination angle.

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