The effects of galaxy shape and rotation on the X-ray haloes of
  early-type galaxies - II. Numerical simulations
  By means of high resolution 2D hydrodynamical simulations, we study the
evolution of the hot ISM for a large set of early-type galaxy models,
characterized by various degrees of flattening and internal rotation. The
galaxies are described by state-of-the-art axisymmetric two-component models,
tailored to reproduce real systems; the dark matter haloes follow the
Navarro-Frenk-White or the Einasto profile. The gas is produced by the evolving
stars, and heated by Type Ia SNe. We find that, in general, the rotation field
of the ISM in rotating galaxies is very similar to that of the stars, with a
consequent negligible heating contribution from thermalization of the ordered
motions. The relative importance of flattening and rotation in determining the
final X-ray luminosity $L_x$ and temperature $T_x$ of the hot haloes is a
function of the galactic mass. Flattening and rotation in low mass galaxies
favour the establishment of global winds, with the consequent reduction of
$L_x$. In medium-to-high mass galaxies, flattening and rotation are not
sufficient to induce global winds, however, in the rotating models the nature
of the gas flows is deeply affected by conservation of angular momentum,
resulting in a reduction of both $L_x$ and $T_x$.
