The Structure and Stability of Relativistic, Differentially Rotating Stars.
Abstract
The stability of axisymmetric, differential rotation in nonmagnetic stars of uniform chemical composition was studied in the context of general relativity theory. Criteria are found for stability against local, linear, axisymmetric perturbations in conducting, viscous stars and in perfect fluid models. When stated in the proper language, the relativistic stability conditions have the same forms as the nonrelativistic conditions. Applications of the stability conditions to models of specific astrophysical objects are discussed. The equations of hydrodynamics in the postNewtonian approximation to general relativity are applied to differentially rotating, barytropic stars. It is shown that the equation of hydrodynamic equilibrium can be integrated to yield a simple algebraic equation, and the gravitational field equations can be written in easily handled integral forms. These facts make possible an iterative scheme of the 'selfconsistent field method' type which can be used to construct numerical models.
 Publication:

Ph.D. Thesis
 Pub Date:
 1975
 Bibcode:
 1975PhDT.........1S
 Keywords:

 Astronomy;
 Astronomical Models;
 Relativistic Theory;
 Stars;
 Stellar Rotation;
 Stellar Structure;
 Hydrodynamics;
 Integral Equations;
 Mathematical Models;
 Newton Theory;
 Stellar Gravitation;
 Astronomy