Relativistic Diskoseismology

Robert Wagoner

Stanford University

October 26,



I shall summarize the results of calculations of the eigenfunctions and eigenfrequencies of normal modes of oscillation trapped within the inner region of their accretion disk by the strong-field gravitational properties of a black hole (or a compact, weakly-magnetized neutron star). The focus will be on the most robust class: the analogue of internal gravity modes in stars. Their frequency which corrresponds to the lowest mode numbers depends 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.

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