A Magnetohydrodynamic Nonradiative Accretion Flow in Three Dimensions
Abstract
We present a global magnetohydrodynamic (MHD) three dimensional simulation of a nonradiative accretion flow originating in a pressure supported torus. The evolution is controlled by the magnetorotational instability which produces turbulence. The flow forms a nearly Keplerian disk. The total pressure scale height in this disk is comparable to the vertical size of the initial torus. Gas pressure dominates only near the equator; magnetic pressure is more important in the surrounding atmosphere. A magnetically dominated bound outflow is driven from the disk. The accretion rate through the disk exceeds the final rate into the hole, and a hot torus forms inside 10 r_g. Hot gas, pushed up against the centrifugal barrier and confined by magnetic pressure, is ejected in a narrow, unbound, conical outflow. The dynamics are controlled by magnetic turbulence, not thermal convection, and a hydrodynamic alpha model is inadequate to describe the flow. The limitations of two dimensional MHD simulations are also discussed.
Keywords
Cite
@article{arxiv.astro-ph/0103522,
title = {A Magnetohydrodynamic Nonradiative Accretion Flow in Three Dimensions},
author = {John F. Hawley and Steven A. Balbus and James M. Stone},
journal= {arXiv preprint arXiv:astro-ph/0103522},
year = {2009}
}
Comments
5 pages, 2 figures, submitted to ApJ Letters. For web version and mpeg animations see http://www.astro.virginia.edu/~jh8h/nraf/