  Theoretical $\Lambda$CDM cosmological models predict a much larger number of
low mass dark matter haloes than has been observed in the Local Group of
galaxies. One possible explanation is the increased difficulty of detecting
these haloes if most of the visible matter is lost at early evolutionary phases
through galactic winds. In this work we study the current models of triggering
galactic winds in dwarf spheroidal galaxies (dSph) from supernovae, and study,
based on 3D hydrodynamic numerical simulations, the correlation of the mass
loss rates and important physical parameters as the dark matter halo mass and
its radial profile, and the star formation rate. We find that the existence of
winds is ubiquitous, independent on the gravitational potential. Our
simulations revealed that the Rayleigh-Taylor Instability (RTI) may play a
major role on pushing matter out of these systems, even for very massive
haloes. The instability is responsible for 5 - 40% of the mass loss during the
early evolution of the galaxy, being less relevant at $t > 200$Myrs. There is
no significant difference in the mass loss rates obtained for the different
dark matter profiles studied (NFW and logarithmic). We have also found a
correlation between the mass loss rate and both the halo mass and the rate of
supernovae, as already reported in previous works. Besides, the epoch in which
most of the baryon galactic matter is removed from the galaxy varies depending
on the SN rate and gravitational potential. The later, combined to the
importance of the RTI in each model, may change our understanding about the
chemical evolution of dwarf galaxies, as well as in the heavy element
contamination of the intergalactic medium at high redshifts.
