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The Dynamical Structure of Nonradiative Black Hole Accretion Flows

Abstract:

We analyze three-dimensional magnetohydrodynamic (MHD) simulations of a nonradiative accretion flow around a black hole using a pseudo-Newtonian potential. The flow originates from a torus initially centered at 100 gravitational (Schwarzschild) radii. Accretion is driven by turbulent stresses generated self-consistently by the magnetorotational instability. The resulting flow has three well-defined dynamical components: a hot, thick, rotationally-dominated Keplerian disk; a surrounding magnet...

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Publication status:
Published

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Publisher copy:
10.1086/340765

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Institution:
University of Oxford
Department:
Oxford, MPLS, Physics, Astrophysics
Role:
Author
Journal:
ASTROPHYSICAL JOURNAL
Volume:
573
Issue:
2
Pages:
738-748
Publication date:
2002-03-19
DOI:
EISSN:
1538-4357
ISSN:
0004-637X
URN:
uuid:64b2e138-0433-4ce1-b06e-7ddab2b3a00d
Source identifiers:
333901
Local pid:
pubs:333901
Keywords:

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