2-TEMPERATURE ACCRETION DISKS WITH WINDS IN A FLUID APPROXIMATION

We use the polytropic relation between pressure and density of wind gases to obtain solutions for optically thin, hot accretion disks with winds. We assume that cooling mechanisms in the disks are bremsstrahlung and Compton scattering. This extends the previous work of Takahara, Rosner, & Kusunose, which did not analyze winds within a self-consistent disk model. We show that the disks have winds for accretion rates higher than approximately 10% of the Eddington rate, depending on the viscosity parameter of the disks and the polytropic exponent of wind gases, gamma-w. The poloidal velocity of winds at the foot-point is shown to be as high as 10% of light speed. We obtain solutions with a mass-loss rate as high as 50% of the accretion rate given at the outer boundary for gamma-w = 5/3. As gamma-w approaches unity, the maximum allowable mass-loss rate decreases for a given accretion rate at the outer boundary. We also numerically show that the winds do not play an effective role to stabilize the disks against perturbations of the proton temperature.