  Some dynamical aspects of gravitational collapse are explored in this paper.
A time-dependent spherically symmetric metric is proposed and the corresponding
Einstein field equations are derived. An ultrarelativistic dust-like
stress-momentum tensor is considered to obtain analytical solutions of these
equations, with a perfect fluid consisting of two purely radial fluxes -the
inwards flux of collapsing matter and the outwards flux of thermally emitted
radiation. Thermal emission is calculated by means of a simplistic but
illustrative model of unintercting collapsing shells. Our results show an
asymptotic approach to a maxiamal spacetime deformation without the formation
of event horizons. Tehe size of the body is slightly larger than the
Schwarzschild radius during most of its lifetime, so that tehre is no
contradiction with either observations or previous theorems concerning black
holes. The relation of the latter with our results is scrutinized in detail.
