A Magnetohydrodynamic Nonradiative Accretion Flow in Three Dimensions

Journal article

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.

Authors: Hawley, J; Balbus, S; Stone, J

• Publication status: Published
• Journal: ASTROPHYSICAL JOURNAL
• Volume: 554
• Issue: 1
• Pages: L49-L52
• Publication date: 2001-03-30
• DOI: 10.1086/320931
• ISSN: 0004-637X
• Keywords: astro-ph