Hydrodynamic Models of Line‐driven Accretion Disk Winds. III. Local Ionization Equilibrium

We present time-dependent numerical hydrodynamic models of line-drivenaccretion disk winds in cataclysmic variable systems and calculate windmass-loss rates and terminal velocities. The models are 2.5-dimensional,include an energy balance condition with radiative heating and coolingprocesses, and includes local ionization equilibrium introducing timedependence and spatial dependence on the line radiation force parameters. Theradiation field is assumed to originate in an optically thick accretion disk.Wind ion populations are calculated under the asumption that local ionizationequilibrium is determined by photoionization and radiative recombination,similar to a photoionized nebula. We find a steady wind flowing from theaccretion disk. Radiative heating tends to maintain the temperature in thehigher density wind regions near the disk surface, rather than coolingadiabatically. For a disk luminosity Ldisk = Lsun, white dwarf mass Mwd = 0.6Msun, and white dwarf radii Rwd = 0.01 Rsun, we obtain a wind mass-loss rate ofdMwind/dt =4E-12 Msun/yr, and a terminal velocity of ~ 3000 km/s. These resultsconfirm the general velocity and density tructures found in our earlierconstant ionization equilibrium adiabatic CV wind models. Further we establishhere 2.5D numerical models that can be extended to QSO/AGN winds where thelocal ionization equilibrium will play a crucial role in the overall dynamics.Comment: 43 pages, 12 figures, to be published in The Astrophysical Journa