  We study the gravitational collapse of a spherically symmetric anisotropic
relativistic star within Einstein theory of gravity making use of one of our
recently developed collapsing stellar models [{\it Astrophys. Space Sci.}
{\bf361} 99 (2016)]. The final state of continual gravitational collapse of a
massive star under regular initial conditions is analyzed in terms of the
formation of black holes. To study the evolution of an anisotropic star
undergoing gravitational collapse, it is assumed that the dissipation process
happens in the form of radial heat-flux. The interior space-time is described
by static metric matched at the boundary with Vaidya metric that describes the
exterior to the radiating star. The initial static configuration is described
by the relativistic solution obtained by Paul and Deb [{\it Astrophys. Space
Sci.} {\bf354} 421 (2014)]. The impact of anisotropy on the dynamical
gravitational collapse of a massive star is studied. The relativistic causal
heat transport equation of the Maxwell-Cattaneo equation is utilized to show
the dependence of anisotropy on the temperature profile of the collapsing
system.
