2007/05/01 by Alexander Shatskiy, A. A. Shatskii · 1 citation
Engineering · Physics and Astronomy · #Cosmology and Gravitation Theories #Material Science and Thermodynamics #Pulsars and Gravitational Waves Research #gr-qc
paper · pdf · doi:10.1134/s1063776107050081
published as J.Exp.Theor.Phys.104:743-750,2007; Zh.Eksp.Teor.Fiz.104:851-859,2007 · 12 pages, 2 figures
openalex publication_date 2007/05/01 · arxiv created 2007/11/02 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
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).