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Radiation hydrodynamic simulations of super-Eddington accretion flows

Published online by Cambridge University Press:  01 August 2006

Ken Ohsuga
Ken Ohsuga*
Affiliation:
Department of Physics, Rikkyo University, Toshimaku, Tokyo 171-8501, Japan email: [email protected]
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Abstract

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We perform the two-dimensional radiation-hydrodynamic simulations to study the radiation pressure-dominated accretion flows around a black hole (BH). Our simulations show that the highly supercritical accretion flow (mass accretion rate is much larger than the critical value) is composed of the disk region and the outflow region above the disk.

The radiation force supports the thick disk and drives the outflow. The photon trapping plays an important role within the disk, reducing the disk luminosity. On the other hand, in the case that mass accretion rate moderately exceeds the critical value, we find that the disk is unstable and exhibits the limit-cycle oscillations. The disk oscillations in our simulations nicely fit to the variation amplitude and duration of quasi-periodic luminosity variations observed in the GRS 1915+105 microquasar.

Keywords

Accretionaccretion disks – black hole physics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 301 - 304
Copyright
Copyright © International Astronomical Union 2007

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