  Starting off with two distinct initially static stellar cores (i) Florides
interior (constant density, vanishing radial pressure) and (ii) Wyman interior
(constant density, nonvanishing radial pressure), we explore the dynamics of
these two models once hydrostatic equilibrium is lost. We show that although
the time of formation of horizon, evolution of the mass and proper radius are
independent of the chosen initially static configurations, there is a
significant difference in the temperature profiles of the radiating bodies as
the collapse proceeds.
