  We study the hydrodynamical evolution of galactic winds in disky dwarf
galaxies moving through an intergalactic medium. In agreement with previous
investigations,we find that when the ram pressure stripping does not disrupt
the ISM, it usually has a negligible effect on the galactic wind dynamics. Only
when the IGM ram pressure is comparable to the central ISM thermal pressure the
stripping and the superwind influence each other increasing the gas removal
rate. In this case several parameters regulate the ISM ejection process, as the
original distribution of the ISM and the geometry of the IGM-galaxy
interaction. When the ISM is not removed by the ram pressure or the wind, it
loses memory of the starburst episode and recovers almost its pre-burst
distribution in a timescale of 50-200 Myr. After this time another star
formation episode becomes, in principle, possible. Evidently, galactic winds
are consistent with a recurrent bursts star formation history.
  Contrary to the ISM content, the amount of the metal-rich ejecta retained by
the galaxy is more sensitive to the ram pressure action. Part of the ejecta is
first trapped in a low density, extraplanar gas produced by the IGM-ISM
interaction, and then pushed back onto the galactic disc. The amount of trapped
metals in a moving galaxy may be up to three times larger than in a galaxy at
rest. This prediction may be tested comparing metallicity of dwarf galaxies in
nearby poor clusters or groups, such as Virgo or Fornax, with the field
counterpart. The sensitivity of the metal entrapment efficiency on the geometry
of the interaction may explain part of the observed scatter in the
metallicity-luminosity relation for dwarf galaxies.
