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

Abstract

We solve the two-dimensional 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 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 $r-\theta$ space. We have found that thermal conduction is 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 disc 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.

20 pages, 10 figures, accepted for publication in ApJ

References in corpus (8)

• Numerical Simulation of Hot Accretion Flows (III): Revisiting wind properties using trajectory approach
• Ultra-fast outflows in radio-loud active galactic nuclei
• Magnetically-Driven Accretion-Disk Winds and Ultra-Fast Outflows in PG1211+143
• Hard-state accretion disk winds from black holes: the revealing case of MAXI J1820+070
• Hot Accretion With Conduction: Spontaneous Thermal Outflows
• On the structure of Accretion Disks with Outflows
• Self-Similar Solution of Hot Accretion Flows with Ordered Magnetic Field and Outflow
• Two-dimensional Inflow-outflow Solution of Supercritical Accretion Flow