  With 2D hydrodynamical simulations, we study the evolution of the hot gas
flows in early-type galaxies, focussing on the effects of galaxy rotation on
the thermal and dynamical status of the ISM. The galaxy is modelled as a
two-component axisymmetric system (stars and dark matter), with a variable
amount of azimuthal velocity dispersion and rotational support; the presence of
a counter rotating stellar disk is also considered. It is found that the ISM of
the rotationally supported (isotropic) model is more prone to thermal
instabilities than the fully velocity dispersion counterpart, while its ISM
temperature and X-ray luminosity are lower. The model with counter rotation
shows an intermediate behaviour.
