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Wave modes from the magnetorotational instability in accretion discs

Authors Giuseppe Di Bernardo
Ulf Torkelsson
Published in IAU Symp. 290: Feeding compact objects: Accretion on all scales, C. Zhang, T. Belloni, M. Méndez & S. Zhang (eds.)
Pages 201-202
ISBN 9781107033795
ISSN 1743-9213
Publication year 2013
Published at Department of Physics (GU)
Pages 201-202
Language en
Keywords Accretion discs, instability, MHD, turbulence, wave methods: numerical
Subject categories High energy astrophysics


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.

Page Manager: Webmaster|Last update: 9/11/2012

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