  We study the effects of pressure anisotropy and heat dissipation in a
spherically symmetric radiating star undergoing gravitational collapse. An
exact solution of the Einstein field equations is presented in which the model
has a Friedmann-like limit when the heat flux vanishes. The behaviour of the
temperature profile of the evolving star is investigated within the framework
of causal thermodynamics. In particular, we show that there are significant
differences between the relaxation time for the heat flux and the relaxation
time for the shear stress.
