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Wave modes from the magnetorotational instability in accretion discs

Published online by Cambridge University Press:  21 February 2013

Giuseppe Di Bernardo  and
Ulf Torkelsson
Giuseppe Di Bernardo
Affiliation:
Department of Physics, University of Gothenburg, SE 412 96 Gothenburg, Sweden email: giuseppe.dibernardo@physics.gu.se, torkel@chalmers.se Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720 email: giuseppe.dibernardo@berkeley.edu
Ulf Torkelsson
Affiliation:
Department of Physics, University of Gothenburg, SE 412 96 Gothenburg, Sweden email: giuseppe.dibernardo@physics.gu.se, torkel@chalmers.se
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Abstract

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The magnetorotational instability (MRI) is widely believed to be the source of turbulence in accretion discs. This turbulence is responsible for the anomalous angular momentum transport in accretion discs. The turbulence will affect other aspects of the dynamics of the disc as well, and we will concentrate on two such issues: a) what kind of oscillations can be excited by the turbulence itself, and b) how the turbulence is interacting with modes that have been excited by some other agent. This is of interest in understanding the quasi-periodic oscillations (QPOs) that have been observed in the X-ray light curves of accreting neutron star and black hole binaries. We carry out local three dimensional (3D) magnetohydrodynamic simulations of a keplerian differentially rotating accretion disc, using a shearing box configuration taking in account the effects of the vertical stratification.

Keywords

Accretion discsinstabilityMHDturbulencewavemethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 201 - 202
Copyright
Copyright © International Astronomical Union 2013

References

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