Two-dimensional inflow-wind solution of black hole accretion with an evenly symmetric magnetic field

Abstract

We solve the two-dimensional magnetohydrodynamic (MHD) equations of black hole accretion with the presence of magnetic field. The field includes a turbulent component, whose role is represented by the viscosity, and a large-scale ordered component. The latter is further assumed to be evenly symmetric with the equatorial plane. The equations are solved in the $r-\theta$ plane of a spherical coordinate by assuming time-steady and radially self-similar. An inflow-wind solution is found. Around the equatorial plane, the gas is inflowing; while above and below the equatorial plane at a certain critical $\theta$ angle, $\theta \sim 47^{\circ }$, the inflow changes its direction of radial motion and becomes wind. The driving forces are analyzed and found to be the centrifugal force and the gradient of gas and magnetic pressure. The properties of wind are also calculated. The specific angular momentum of wind is found to be significantly larger than that of inflow, thus wind can transfer angular momentum outward. These analytical results are compared to those obtained by the trajectory analysis based on MHD numerical simulation data and good agreements are found.

9 pages, 4 figures, accepted by MNRAS

References in corpus (8)

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• The Effect of Large Scale Magnetic Field on Outflow in ADAFs: an Odd Symmetry Configuration
• On the wind production from hot accretion flows with different accretion rates
• The Effects of Magnetic Field Strength on Properties of Wind Generated from Hot Accretion Flow
• The 2D disk structure with advective transonic inflow-outflow solutions around black holes
• Radiation-driven outflows in AGNs: Revisiting feedback effects of scattered and reprocessed photons
• Two-dimensional Inflow-outflow Solution of Supercritical Accretion Flow
• The effects of toroidal magnetic field on the vertical structure of hot accretion flows
• Standing shocks in magnetized advection accretion flows onto a rotating black hole
• Two-dimensional Inflow-Wind Solution of Hot Accretion Flow. I. Hydrodynamics
• The influence of outflow in supercritical accretion flows
• Self-similar solutions for finite size advection-dominated accretion flows
• Three-dimensional simulations of accretion flow in the progenitor of Tycho's supernova
• Anchoring polar magnetic field in a stationary thick accretion disk
• Self-similar solution of hot accretion flow: the role of kinematic viscosity coefficient