  We model a compact radiant star that undergoes gravitational collapse from a
certain initial static configuration until it becomes a black hole. The star
consists of a fluid with anisotropy in pressures, bulk viscosity, in addition
to the radial heat flow. A solution of Einstein's field equations with temporal
dependence was presented to study the dynamic evolution of physical quantities,
such as the mass-energy function, the luminosity seen by an observer at
infinity and the heat flow. We checked the acceptability conditions of the
initial static configuration to obtain a range of mass-to-radius ratio in which
the presented star model is physically reasonable. The energy conditions were
analyzed for the dynamic case, in order to guarantee that the model is composed
of a physically acceptable fluid within the range of the mass-to-radius ratio
obtained for the static configuration or if they will be modified during the
collapse
