Numerical Models of Viscous Accretion Flows Near Black Holes

Details Numerical Models of Viscous Accretion Flows Near Black Holes Numerical Models of Viscous Accretion Flows Near Black Holes

2002-04-03

arxiv.org/abs/astro-ph/0204045v1

Astronomy and Astrophysics

Astrophysics

14 pages, 4 figures, 2 tables, to appear in v573 n2 pt1 ApJ July 10, 2002

Scientific paper

10.1086/340761

We report on a numerical study of viscous fluid accretion onto a black hole. The flow is axisymmetric and uses a pseudo-Newtonian potential to model relativistic effects near the event horizon. The numerical method is a variant of the ZEUS code. As a test of our numerical scheme, we are able to reproduce results from earlier, similar work by Igumenshchev and Abramowicz and Stone et al. We consider models in which mass is injected onto the grid as well as models in which an initial equilibrium torus is accreted. In each model we measure three ``eigenvalues'' of the flow: the accretion rate of mass, angular momentum, and energy. We find that the eigenvalues are sensitive to r_{in}, the location of the inner radial boundary. Only when the flow is always supersonic on the inner boundary are the eigenvalues insensitive to small changes in r_{in}. We also report on the sensitivity of the results to other numerical parameters.

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