On the structure and stability of rapidly rotating fluid bodies in general relativity. III. Beyond the angular velocity peak.
Abstract
A method previously described by Butterworth and Ipser for constructing models of rapidly rotating fluid bodies in general relativity is modified to enable construction of solutions whose sources are very highly flattened. In particular, solutions with increasing oblateness and decreasing angular velocity are exhibited. Also, a discussion is given of the possible association of the termination of relativistic sequences by equatorial shedding and the first secular axisymmetric instability of the Maclaurin spheroids.
 Publication:

The Astrophysical Journal
 Pub Date:
 July 1979
 DOI:
 10.1086/157183
 Bibcode:
 1979ApJ...231..219B
 Keywords:

 Angular Velocity;
 Dynamic Stability;
 Relativistic Effects;
 Rotating Bodies;
 Rotating Fluids;
 Stellar Rotation;
 Angular Momentum;
 Astronomical Models;
 Axisymmetric Bodies;
 Fluid Dynamics;
 Graphs (Charts);
 Numerical Analysis;
 Polynomials;
 Relativity;
 Rotating Spheres;
 Secular Variations;
 Astrophysics;
 Fluid Spheres:Rotation;
 Fluid Spheres:Stability