Dynamics of phantom matter

Abstract

A spherically symmetric evolution model of self-gravitating matter with the equation of state p = −(1 + δ)ɛ (where δ = const) is considered. The equations of the model are written in the frame of reference co-moving with matter. A criterion for the existence and formation of a horizon is defined. Part of the Einstein equations is integrated analytically. The initial conditions and the constraints imposed on these conditions in the presence of a horizon are determined. For small δ, an analytic solution to spherically symmetric time-dependent Einstein equations is obtained. Conditions are determined under which the dynamics of matter changes from collapse to expansion. Characteristic times of the evolution of the system are evaluated. It is proved that the accretion of phantom matter (for δ > 0) onto a black hole leads to the decreases of the horizon radius of the black hole (i.e., the black hole is dissolved).