Galactic winds and circulation of the interstellar medium in dwarf galaxies

We study, through 2D hydrodynamical simulations, the feedback of a starburst on the ISM of typical gas rich dwarf galaxies. The main goal is to address the circulation of the ISM and metals following the starburst. We assume a single-phase rotating ISM in equilibrium in the galactic potential generated by a stellar disk and a spherical dark halo. The starburst is assumed to occur in a small volume in the center of the galaxy, and it generates a mechanical power of 3.8e39 erg/s or 3.8e40 erg/s for 30 Myr. We found, consistently with previous investigations, that the galactic wind is not very effective in removing the ISM. The metal rich stellar ejecta, instead, may be efficiently expelled from the galaxy and dispersed in the intergalactic medium. Moreover, we found that the central region of the galaxy is always replenished with cold and dense gas after a few 100 Myr from the starbust, achieving the requisite for a new star formation event in 0.5-1 Gyr. The hydrodynamical evolution of galactic winds is thus consistent with the episodic star formation regime suggested by many chemical evolution studies. We also discuss the X-ray emission of these galaxies and find that the observable (emission averaged) abundance of the hot gas underestimates the real one if thermal conduction is effective. This could explain the very low hot gas metallicities estimated in starburst galaxies.