Spherical collapse of a nonrotating perfect fluid in the non-symmetric theory of gravitation

Abstract

A set of time-dependent differential equations governing the behaviour of a spherically symmetric non-rotating perfect fluid in the non-symmetric theory of gravitation (NGT), is derived in a form suitable for numerical computations. This is then applied to the pressureless collapse of such a fluid. If the Newtonian potential does not exceed a certain value, and if the NGT potential is large enough, the collapse stops and reverses itself into an expansion before the Schwarzschild horizon is reached. A solution is presented for the case where the attractive tensor component of the NGT force is negligible. Bounds are found on the Newtonian potential and the ratio of NGT to Newtonian potentials within which the bounce phenomenon must occur.

Gravitational waves from an axi-symmetric source in the Nonsymmetric Gravitational Theory

“…Since NGT was introduced [10] there have been few analytic solutions of the field equations published. The exact solutions known to date include the spherically symmetric vacuum case [11], the spherically symmetric interior case [12,13] and Bianchi type I cosmological solutions with and without matter [14,15]. This, at least in part, follows from the fact that deriving NGT field equations relevant for particular cases of interest is not as technically simple as may be suggested by its superficial similarity to the corresponding GR situations.…”