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Relativistic Diskoseismology

Published online by Cambridge University Press:  12 April 2016

Robert V. Wagoner
Robert V. Wagoner*
Affiliation:
Department of Physics and Center for Space Science and Astrophysics, Stanford University, Stanford, CA 94305–4060, USA

Abstract

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We will summarize results of relativistic calculations of the eigenfunctions and eigenfrequencies of modes of oscillation trapped within the inner region of thin accretion disks by non-Newtonian gravitational properties of a black hole (or a compact, weakly-magnetized neutron star). The focus will be on the most observable, robust, and best-studied class: the analogue of (internal) gravity modes in stars. The frequencies of the corresponding peaks in the power spectrum of the resulting luminosity modulations depend almost entirely upon only the mass and angular momentum of the black hole. The frequency width also depends upon the viscosity parameter of the disk. Searches for such features are being carried out by the RXTE satellite.

Type
Part 7. Local and Global Instabilities and Disk Perturbations
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 300 - 310
Copyright
Copyright © Astronomical Society of the Pacific 1997

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