Relativistic Diskoseismology

Details Relativistic Diskoseismology Relativistic Diskoseismology

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.7615l&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #76.15; Bulletin of the American Astronomical Society, Vol. 28, p.1373

Astronomy and Astrophysics

Astronomy

Scientific paper

We review the relativistic results for ``diskoseismic" modes of oscillation which are trapped within thin accretion disks by non-Newtonian gravitational properties of a black hole. In particular, we will present results for both ``g-modes", which are the rough analogue of (internal) gravity modes in stars and are expected to be the most robust and observable class of modes, and acoustic ``p-modes", including the most recent investigations of the latter which may exist in a large region of the disk which extends to the outer boundary. The most definitive property of the g-modes is that the resulting eigenfrequencies depend almost entirely upon only the mass and angular momentum of the black hole. Such a feature has recently been detected by RXTE in the power spectrum of the luminosity modulations of the BHC GRS 1915+105. With a frequency of 67 Hz, this feature remained stable in frequency despite appreciable luminosity fluctuations. We consider the possibility that this feature can be attributed to a g-mode in an accretion disk about a 10.6 M_sun (non-rotating) - 36.3 M_sun (maximally rotating) black hole.

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