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New global 3D MHD simulations of black hole disk accretion and outflows

Published online by Cambridge University Press:  01 November 2008

Peter B. Dobbie ,
Zdenka Kuncic ,
Geoffrey V. Bicknell  and
Raquel Salmeron
Peter B. Dobbie
Affiliation:
School of Physics, University of Sydney, NSW 2006, Australia email: p.dobbie@physics.usyd.edu.au
Zdenka Kuncic
Affiliation:
School of Physics, University of Sydney, NSW 2006, Australia email: p.dobbie@physics.usyd.edu.au
Geoffrey V. Bicknell
Affiliation:
Research Centre for Astronomy and Astrophysics, Australian National University, ACT 2611, Australia
Raquel Salmeron
Affiliation:
Research Centre for Astronomy and Astrophysics, Australian National University, ACT 2611, Australia
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Abstract

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It is widely accepted that quasars and other active galactic nuclei (AGN) are powered by accretion of matter onto a central supermassive black hole. While numerical simulations have demonstrated the importance of magnetic fields in generating the turbulence believed necessary for accretion, so far they have not produced the high mass accretion rates required to explain the most powerful sources. We describe new global 3D simulations we are developing to assess the importance of radiation and non-ideal MHD in generating magnetized outflows that can enhance the overall rates of angular momentum transport and mass accretion.

Keywords

Accretion – accretion disks – magnetic fields – MHD – radiative transfer – turbulence – methods: numerical – galaxies: active, jets, magnetic fields, nuclei – (galaxies:) quasars: general – x-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 129 - 130
Copyright
Copyright © International Astronomical Union 2009

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