Galactic winds and circulation of the interstellar medium in dwarf galaxies

We study, through 2D hydrodynamical simulations, the feedback of a starburs t on the ISM of typical gas-rich dwarf galaxies. The main goal is to addres s the circulation of the ISM and metals following the starburst. We assume a single-phase rotating ISM in equilibrium in the galactic potential genera ted by a stellar disc and a spherical dark halo. The starburst is assumed t o occur in a small volume in the centre of the galaxy, and it generates a m echanical power of 3.8 x 10(39) or 3.8 x 10(40) erg s(-1) for 30 Myr. We fi nd, in accordance with previous investigations, that the galactic wind is n ot very effective in removing the ISM. The metal-rich stellar ejecta, howev er, can be efficiently expelled from the galaxy and dispersed in the interg alactic medium. Moreover, we find that the central region of the galaxy is always replenish ed with cold and dense gas a few 100 million years after the starburst, ach ieving the requisite for a new star formation event in;approximate to 0.5-1 Gyr, The hydrodynamical evolution of galactic winds is thus consistent wit h the episodic star formation regime suggested by many chemical evolution s tudies. We also discuss the X-ray emission of these galaxies and find that the obse rvable (emission-averaged) abundance of the hot gas underestimates the real one if thermal conduction is effective. This could explain the very low ho t-gas metallicities estimated in starburst galaxies.