Gravitational Collapse in Free Fall of a Slowly Rotating Star
Abstract
The gravitational collapse of a slowly rotating star with small deviations from spherical symmetry is studied. The exterior metric is chosen to be the Kerr metric in synchronous coordinates discarding terms of order (a/r)^{2}. Interior geometry is constructed by adding an offdiagonal term in first order ofa to the exact solution of the nonrotating case. This term is determined in part by requiring the validity of the junction conditions at the star's surface and by demanding that the angular momentum of the source is equal toM A, in agreement with the value measured by a distant observer. The resulting stressenergy tensor describes a homogeneous, pressureless, ideal fluid which rotates nonuniformly relative to the synchronous frame which is no longer comoving the stellar matter.
 Publication:

Astrophysics and Space Science
 Pub Date:
 March 1993
 DOI:
 10.1007/BF00627195
 Bibcode:
 1993Ap&SS.201..223T
 Keywords:

 Black Holes (Astronomy);
 Gravitational Collapse;
 Stellar Evolution;
 Stellar Rotation;
 Computational Astrophysics;
 Cosmic Dust;
 Ideal Fluids;
 Stellar Interiors;
 Stellar Models;
 Stress Tensors;
 Astrophysics