Gravitational Collapse without a Remnant

Abstract

We investigate the gravitational collapse of a spherically symmetric, inhomogeneous star, which is described by a perfect fluid with heat flow and satisfies the equation of state p = ρ/3 or p = Cρ γ at its center. Different from the ordinary process of gravitational collapsing, the energy of the whole star is emitted into space. And the remaining spacetime is a Minkowski one at the end of the process.

Local behaviour of evaporating stars and black holes around the total evaporation event

“…A spherically symmetric timelike hypersurface ( ū(τ ), R(τ )) (where τ is a future-directed time coordinate defined only on the hypersurface) is timelike and future directed if, and only if, χ u + 2 Ṙ > 0 (11) and u > 0, where dots stand for derivatives with respect to τ .…”

“…Therefore, these models do not need to be in a stationary equilibrium configuration nor to bounce to avoid the formation of a singularity. Along this line, other authors have proposed new evaporating models with different matter fields [9], different exact solutions of Einstein's equations for non-perfect fluids with heat flow [10] or different equations of state [11]. Recently [12], a new mechanism for ejecting matter (based on the mini-super-space loop quantum gravity formalism) has been proposed with the aim of creating this kind of evaporating singularity free models.…”