The Oscillations of Rapidly Rotating Newtonian Stellar Models
Abstract
A method is described for solving the equations that govern the oscillations of rapidly rotating inhomogeneous Newtonian stellar models. A covariant reformulation of the general pulsation equations is presented, which reduces them to a single scalar equation for a single potential. From this potential, all of the properties of the normal mode may be deduced. The techniques developed to solve this complicated eigenvalue problem numerically are described, and solutions to this equation are presented for the l = m fmodes of rigidly rotating stellar models having polytropic equations of state.
 Publication:

The Astrophysical Journal
 Pub Date:
 May 1990
 DOI:
 10.1086/168757
 Bibcode:
 1990ApJ...355..226I
 Keywords:

 Stellar Models;
 Stellar Oscillations;
 Stellar Rotation;
 Computational Astrophysics;
 Equations Of State;
 Polytropic Processes;
 Astrophysics;
 HYDRODYNAMICS;
 STARS: INTERIORS;
 STARS: PULSATION;
 STARS: ROTATION