期刊
ASTROPHYSICAL JOURNAL
卷 554, 期 1, 页码 L49-L52出版社
UNIV CHICAGO PRESS
DOI: 10.1086/320931
关键词
accretion, accretion disks; black hole physics; instabilities; MHD
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 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 10r(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.
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