  We will summarize results of calculations of the modes of oscillation trapped
within the inner region of accretion disks by the strong-field gravitational
properties of a black hole (or a compact, weakly-magnetized neutron star).
Their driving and damping will also be addressed. The focus will be on the most
observable class: the analogue of internal gravity modes in stars. Their
frequencies which corrrespond to the lowest mode numbers depend 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.
