Two-dimensional Inflow-wind Solution of Hot Accretion Flow. I. Hydrodynamics

We solve the 2D hydrodynamic equations of hot accretion flow in the presence of the thermal conduction. The flow is assumed to be in steady state and axisymmetric, and a self-similar approximation is adopted in the radial direction. In this hydrodynamic study, we consider the viscous stress tensor to mimic the effects of the magnetorotational instability for driving angular momentum. We impose the physical boundary conditions at both the rotation axis and the equatorial plane and obtain the solutions in the full r -θ space. We have found that thermal conduction is an indispensable term for investigating the inflow-wind structure of the hot accretion flows with very low mass accretion rates. One of the most interesting results here is that the disk is convectively stable in hot accretion mode and in the presence of the thermal conduction. Furthermore, the properties of wind and also its driving mechanisms are studied. Our analytical results are consistent with previous numerical simulations of hot accretion flow.