On the Perturbations of Viscous Rotating Newtonian Fluids

Details On the Perturbations of Viscous Rotating Newtonian Fluids On the Perturbations of Viscous Rotating Newtonian Fluids

2000-02-22

arxiv.org/abs/astro-ph/0002419v1

Astronomy and Astrophysics

Astrophysics

Accepted for publication by The Astrophysical Journal. 11 pages, no figures

Scientific paper

10.1086/309060

The perturbations of weakly-viscous, barotropic, non-self-gravitating, Newtonian rotating fluids are analyzed via a single partial differential equation. The results are then used to find an expression for the viscosity-induced normal-mode complex eigenfrequency shift, with respect to the case of adiabatic perturbations. However, the effects of viscosity are assumed to have been incorporated in the unperturbed (equilibrium) model. This paper is an extension of the normal-mode formalism developed by Ipser & Lindblom for adiabatic pulsations of purely-rotating perfect fluids. The formulas derived are readily applicable to the perturbations of thin and thick accretion disks. We provide explicit expressions for thin disks, employing results from previous relativistic analyses of adiabatic normal modes of oscillation. In this case, we find that viscosity causes the fundamental p- and g- modes to grow while the fundamental c-mode could have either sign of the damping rate.

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