Hydrodynamic models of line-driven accretion disk winds. III. Local ionization equilibrium

We present time-dependent numerical hydrodynamic models of line-driven accretion disk winds in cataclysmic variable systems and calculate wind mass-loss rates and terminal velocities. The models are 2.5-dimensional, include an energy balance condition with radiative heating and cooling processes, and include local ionization equilibrium introducing time dependence and spatial dependence on the line radiation force parameters. The radiation field is assumed to originate in an optically thick accretion disk. Wind ion populations are calculated under the assumption that local ionization equilibrium is determined by photoionization and radiative recombination, similar to a photoionized nebula. We find a steady wind owing from the accretion disk. Radiative heating tends to maintain the temperature in the higher density wind regions near the disk surface, rather than cooling adiabatically. For a disk luminosity L-disk=L-circle dot, white dwarf mass M-wd=0.6 M-circle dot, and white dwarf radii R-wd=0.01 R-circle dot, we obtain a wind mass-loss rate of (M)over dot(wind)=4x10(-12) M-circle dot yr(-1) and a terminal velocity of similar to3000 km s(-1). These results confirm the general velocity and density structures found in our earlier constant ionization equilibrium adiabatic cataclysmic variable wind models. Further, we establish here 2.5-dimensional numerical models that can be extended to QSO/AGN winds where the local ionization equilibrium will play a crucial role in the overall dynamics.