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We present here numerical hydrodynamic simulations of line-driven accretiondisk winds in cataclysmic variable systems. We calculate wind mass-loss rate,terminal velocities, and line profiles for CIV (1550 A) for various viewingangles. The models are 2.5-dimensional, include an energy balance condition,and calculate the radiation field as a function of position near an opticallythick accretion disk. The model results show that centrifugal forces producecollisions of streamlines in the disk wind which in turn generate an enhanceddensity region, underlining the necessity of two dimensional calculations wherethese forces may be represented. For disk luminosity Ldisk = Lsun, white dwarfmass Mwd = 0.6 Msun, and white dwarf radii Rwd = 0.01 Rsun, we obtain a windmass-loss rate of dMwind/dt = 8.0E-12 Msun/yr, and a terminal velocity of ~3000km/s. The line profiles we obtain are consistent with observations in theirgeneral form, in particular in the maximum absorption at roughly half theterminal velocity for the blue-shifted component, in the magnitudes of the windvelocities implied by the absorption components, in the FWHM of the emissioncomponents, and in the strong dependence in inclination angle.Comment: 67 pages, 28 Postscript figures, uses aasms4.sty and epsf.st

Hydrodynamic Models of Line‐driven Accretion Disk Winds. II. Adiabatic Winds from Nonisothermal Disks