The Search for Diskoseismic Modes in Three-Dimensional Magnetohydrodynamic Simulations of Black Hole Accretion Disks

Details The Search for Diskoseismic Modes in Three-Dimensional Magnetohydrodynamic Simulations of Black Hole Accretion Disks The Search for Diskoseismic Modes in Three-Dimensional Magnetohydrodynamic Simulations of Black Hole Accretion Disks

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.1108o&link_type=abstract

American Astronomical Society, HEAD meeting #11, #11.08; Bulletin of the American Astronomical Society, Vol. 41, p.672

Astronomy and Astrophysics

Astronomy

Scientific paper

Since the advent of the Rossi X-Ray Timing Explorer, high-frequency quasi-periodic oscillations (HFQPOs) have been observed in multiple galactic black hole binary systems. Because the high ( 100 Hz) frequencies are comparable in magnitude to inner accretion disk orbital frequencies, the correct interpretation of this phenomenon could tell us much about the innermost regions of accretion disks and the black holes they orbit. One natural explanation is that HFQPOs correspond to global disk oscillation modes, but the supporting evidence from numerical simulations of global accretion disks is currently ambiguous at best. On one hand, simulations of thin, viscous, hydrodynamic disks show clear signatures of trapped global modes that could potentially produce the observed HFQPOs. Full three-dimensional magnetohydrodynamic (MHD) simulations, however, have failed thus far to produce convincing, persistent, identifiable HFQPOs. The presence of turbulence driven by the magnetorotational instability certainly complicates the detection of HFQPOs in these models, but it is not yet clear that trapped modes persist in MHD disks at all. We report here on high resolution, global, MHD accretion disk simulations designed specifically to search for diskoseismic modes that may only be detectable over sufficiently long timescales.

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