Relativistic Diskoseismology

Abstract

We will summarize results of calculations of the modes of oscillation trapped within the inner region of accretion disks by the strong-field gravitational properties of a black hole (or a compact, weakly-magnetized neutron star). Their driving and damping will also be addressed. The focus will be on the most observable class: the analogue of internal gravity modes in stars. Their frequencies which corrrespond to the lowest mode numbers depend almost entirely upon only the mass and angular momentum of the black hole. Such a feature may have been detected in the X-ray power spectra of two galactic `microquasars', allowing the angular momentum of the black hole to be determined in one case.

To be published in Physics Reports, proceedings of the conference Astrophysical Fluids: From Atomic Nuclei to Stars and Galaxies; 10 pages, 5 postscript figures

References in corpus (4)

• Black Hole Spin in X-Ray Binaries: Observational Consequences
• Optical Observations of GRO J1655-40 in Quiescence I: A Precise Mass for the Black Hole Primary
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• The 67 Hz Feature in the Black Hole Candidate GRS 1915+105 as a Possible ``Diskoseismic'' Mode

Cited by in corpus (109)

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• Evidence for Harmonic Relationships in the High Frequency QPOs of XTE J1550-564 and GRO J1655-40
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• The X-ray Outburst of H1743-322: High-Frequency QPOs with a 3:2 Frequency Ratio
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