Perturbation Methods for the Calculation of Gravitational Waves from Slightly Nonspherical Spacetimes with Applications to Stellar Core Collapse.
Abstract
A method for the calculation of gravitational radiation from perturbations of spherically symmetric, realistic background stellar models is presented. The numerical background hydrodynamic code is based on a scheme developed by May and White, is fully relativistic, and can be used with any equation of state. Special emphasis will be placed on evenparity gravitational perturbations of the Einstein equations, but oddparity perturbations will also be studied. For the oddparity perturbations, based on the work of Moore, numerical results are presented for dust collapse to a black hole and for stellar collapse models designed to simulate a type II supernova. In this case, we find that oddparity perturbations of such models are capable of radiating up to 10^{ 7} stellar masses in gravitational radiation energy. For the evenparity perturbations, preliminary results are presented for dust collapse and for stellar collapse models with a polytropic equation of state. The polytropic models do not well represent current supernova models, but they do provide a basis for comparison of the even and oddparity perturbations under relativistic conditions in a collapsing star with a polytropic equation of state. For such polytropic stellar models we find that evenparity perturbations are capable of radiating an order of magnitude more in gravitational wave energy than corresponding odd parity perturbations.
 Publication:

Ph.D. Thesis
 Pub Date:
 1988
 Bibcode:
 1988PhDT........13S
 Keywords:

 Physics: Astronomy and Astrophysics;
 A Stars;
 Black Holes (Astronomy);
 Equations Of State;
 Gravitational Waves;
 Hydrodynamics;
 Perturbation;
 Stellar Models;
 Stellar Radiation;
 Supernovae;
 Collapse;
 Dust;
 Stars;
 Astrophysics