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The dynamical structure of nonradiative black hole accretion flows

Abstract:

We analyze three-dimensional magnetohydrodynamic 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 magnetized c...

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Publisher copy:
10.1086/340765
Publisher:
Institute of Physics Publishing
Journal:
Astrophysical Journal More from this journal
Volume:
573
Issue:
2 I
Pages:
738-748
Publication date:
2002-07-10
DOI:
EISSN:
1538-4357
ISSN:
0004-637X
Language:
English
Keywords:
Pubs id:
pubs:334579
UUID:
uuid:081e7bdc-d491-4edb-a1c2-5ce6f2eeaf92
Local pid:
pubs:334579
Source identifiers:
334579
Deposit date:
2015-01-08

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