Radiation from slightly nonspherical models of gravitational collapse
Abstract
The paper examines the first and second order perturbations of the OppenheimerSnyder model of spherical pressureless collapse to a Schwarzschild or slowly rotating Kerr black hole. The first and second order perturbation problems are formulated in terms of suitable gauge invariant quantities and the relevant perturbation equations are solved numerically for some reasonable initial conditions. Waveforms, spectra, and total energies emitted are computed for a variety of representative collapses. The main advantage of this approach is that the perturbation equations are reduced (by an expression in tensor harmonics) to a partial differential system in only two independent variables, and a considerable decoupling of this system is achieved through the use of gauge invariants.
 Publication:

Sources of Gravitational Radiation
 Pub Date:
 1979
 Bibcode:
 1979sgrr.work..231M
 Keywords:

 Astronomical Models;
 Black Holes (Astronomy);
 Gravitational Collapse;
 Cosmology;
 Gravitational Waves;
 Perturbation Theory;
 Waveforms;
 Astrophysics