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By means of high resolution 2D hydrodynamical simulations, we study theevolution of the hot ISM for a large set of early-type galaxy models,characterized by various degrees of flattening and internal rotation. Thegalaxies are described by state-of-the-art axisymmetric two-component models,tailored to reproduce real systems; the dark matter haloes follow theNavarro-Frenk-White or the Einasto profile. The gas is produced by the evolvingstars, and heated by Type Ia SNe. We find that, in general, the rotation fieldof the ISM in rotating galaxies is very similar to that of the stars, with aconsequent negligible heating contribution from thermalization of the orderedmotions. The relative importance of flattening and rotation in determining thefinal X-ray luminosity $L_x$ and temperature $T_x$ of the hot haloes is afunction of the galactic mass. Flattening and rotation in low mass galaxiesfavour the establishment of global winds, with the consequent reduction of$L_x$. In medium-to-high mass galaxies, flattening and rotation are notsufficient to induce global winds, however, in the rotating models the natureof the gas flows is deeply affected by conservation of angular momentum,resulting in a reduction of both $L_x$ and $T_x$.

The effects of galaxy shape and rotation on the X-ray haloes of early-type galaxies - II. Numerical simulations