  In this paper we revise two classical examples of Relativistic Hydrodynamics
in order to illustrate in detail the numerical methods commonly used in fluid
dynamics, specifically those designed to deal with shocks, which are based on a
finite volume approximation. The two cases we consider are the relativistic
blast wave problem and the evolution of a Tolman-Oppenheimer-Volkoff star
model, in spherical symmetry. In the first case we illustrate the
implementation of relativistic Euler's equations on a fixed background
space-time, whereas in the second case we also show how to couple the evolution
of the fluid to the evolution of the space-time.
