Astronomy and Astrophysics – Astrophysics
Scientific paper
2002-03-19
Astronomy and Astrophysics
Astrophysics
Accepted for Publication in the Astrophysical Journal. For a web version see http://www.astro.virginia.edu/VITA/papers/nraf2/
Scientific paper
10.1086/340765
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 magnetized corona with vigorous circulation and outflow; and a magnetically-confined jet along the centrifugal funnel wall. Inside of 10 gravitational radii, the disk becomes very hot, more toroidal, and highly intermittent. These results contrast sharply with quasi-spherical, self-similar viscous models. There are no significant dynamical differences between simulations that include resistive heating and those that do not. We conclude by deducing some simple radiative properties of our solutions, and apply the results to the accretion-powered Galactic center source Sgr A*.
Balbus Steven A.
Hawley John F.
No associations
LandOfFree
The Dynamical Structure of Nonradiative Black Hole Accretion Flows does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The Dynamical Structure of Nonradiative Black Hole Accretion Flows, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Dynamical Structure of Nonradiative Black Hole Accretion Flows will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-620574