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Dynamics of radiatively inefficient flows accreting onto radiatively efficient black hole objects

Published online by Cambridge University Press:  01 August 2006

Daniel Proga
Daniel Proga*
Affiliation:
Department Physics, University of Nevada, Las Vegas, Las Vegas, NV 89154, USA email: [email protected]
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Abstract

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I present results from numerical simulations of gas dynamics outside luminous accretion disks in active galactic nuclei. The gas, gravitationally captured by a super massive black hole, can be driven away by the energy and momentum of the radiation emitted during black hole accretion. Assuming axisymmetry, I study how the mass accretion and outflow rates, and the flow dynamics respond to changes in radiation heating relative to radiation pressure.

I find that for a 108 M⊙ black hole with the accretion luminosity of 0.6 of the Eddington luminosity the flow settles into a steady state and has two components: (1) an equatorial inflow and (2) a bipolar inflow/outflow with the outflow leaving the system along the disk rotational axis. The inflow is a realization of a Bondi–like accretion flow. The second component is an example of a non-radial accretion flow which becomes an outflow once it is pushed close to the rotational axis where thermal expansion and radiation pressure accelerate it outward.

The main result of this preliminary work is that although the above two-component solution is robust, its properties are sensitive to the geometry and spectral energy distribution of the radiation field.

Keywords

Accretionaccretion disks – methods: numerical – hydrodynamics
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. 165 - 169
Copyright
Copyright © International Astronomical Union 2007

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