2000/02/22 by Manuel Ortega-Rodríguez, Manuel Ortega-Rodriguez, Robert V. Wagoner · 20 citations
Physics and Astronomy · #Adiabatic process #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Barotropic fluid #Classical mechanics #Mechanics #Newtonian fluid #Oscillation (cell signaling) #Perturbation (astronomy) #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Thermodynamics #Viscosity #Volume viscosity #astro-ph
paper · pdf · doi:10.1086/309060
published in The Astrophysical Journal 537(2), 922-926 (IOP Publishing) · Accepted for publication by The Astrophysical Journal. 11 pages, no figures
arxiv created 2000/02/22 · openalex publication_date 2000/07/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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 formulae 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.