Diskoseismology: Probing accretion disks. II - G-modes, gravitational radiation reaction, and viscosity

Details Diskoseismology: Probing accretion disks. II - G-modes, gravitational radiation reaction, and viscosity Diskoseismology: Probing accretion disks. II - G-modes, gravitational radiation reaction, and viscosity

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...393..697n&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 393, no. 2, July 10, 1992, p. 697-707. Research supported by U.S. Navy.

Astronomy and Astrophysics

Astronomy

75

Accretion Disks, Gravitational Effects, Relativistic Theory, Stellar Oscillations, Black Holes (Astronomy), Partial Differential Equations, Perturbation Theory

Scientific paper

A scalar potential is used to derive a single partial differential equation governing the oscillation of a disk. The eigenfunctions and eigenfrequencies of a variety of disk models are found to fall into two main classes which are analogous to the p-modes and g-modes in the sun. Specifically, the eigenfunctions and eigenfrequencies of isothermal disks are computed, and the way in which these results can be generalized to other disk models is indicated. The (assumed) relatively small rates of growth or damping of the modes due to various mechanisms, in particular gravitational radiation reaction and parameterized models of viscosity are also computed. It is found that for certain parameters the p-modes are unstable to gravitational radiation reaction (CFS instability), while both the p-modes and g-modes are unstable to viscosity unless highly anisotropic viscosity models are considered.

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