Oscillations of vertically integrated relativistic tori -II. Axisymmetric modes in a Kerr spacetime

Details Oscillations of vertically integrated relativistic tori -II. Axisymmetric modes in a Kerr spacetime Oscillations of vertically integrated relativistic tori -II. Axisymmetric modes in a Kerr spacetime

2004-07-30

arxiv.org/abs/astro-ph/0407642v1

Mon.Not.Roy.Astron.Soc. 354 (2004) 1040-1052

Astronomy and Astrophysics

Astrophysics

13 pages, MNRAS, in press

Scientific paper

10.1111/j.1365-2966.2004.08265.x

This is the second of a series of papers investigating the oscillation properties of relativistic, non-selfgravitating tori orbiting around black holes. Extending the work done in a Schwarzschild background, we here consider the axisymmetric oscillations of vertically integrated tori in a Kerr spacetime. The tori are modeled with a number of different non-Keplerian distributions of specific angular momentum and we discuss how the oscillation properties depend on these and on the rotation of the central black hole. We first consider a local analysis to highlight the relations between acoustic and epicyclic oscillations in a Kerr spacetime and subsequently perform a global eigenmode analysis to compute the axisymmetric p modes. In analogy with what found in a Schwarzschild background, these modes behave as sound waves that are modified by rotation and are globally trapped in the torus. For constant distributions of specific angular momentum, the eigenfrequencies appear in a sequence 2:3:4:... which is essentially independent of the size of the disc and of the black hole rotation. For non-constant distributions of angular momentum, on the other hand, the sequence depends on the properties of the disc and on the spin of the black hole, becoming harmonic for sufficiently large tori. We also comment on how p modes could explain the high frequency quasi-periodic oscillations observed in low-mass X-ray binaries with a black hole candidate and the properties of an equivalent model in Newtonian physics.

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