Previous abstract Next abstract

Session 76 - Cataclysmic Variables and Accretion Disks.
Display session, Wednesday, January 15
Metropolitan Ballroom,

[76.15] Relativistic Diskoseismology

D. E. Lehr, R. V. Wagoner, A. S. Silbergleit (Stanford U.), M. A. Nowak, M. C. Begelman (JILA, U. Colorado)

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_ødot (non-rotating) - 36.3 M_ødot (maximally rotating) black hole.

If you would like more information about this abstract, please follow the link to This link was provided by the author. When you follow it, you will leave the the Web space for this meeting; to return, you should use the Back button on your browser.

Program listing for Wednesday