Tidal tails, resulting from the interactions of large
galaxies, can create self-gravitating structures which are the seeds
of dwarf galaxies.  In these galaxies, commonly known as Tidal Dwarf
Galaxies, the Dark Matter (DM) content is very small, which makes them
more vulnerable to stellar feedback.  In order to study the formation
and the evolution of Tidal Dwarf Galaxies, a fundamental step is
therefore to understand whether a model galaxy without DM can sustain
the feedback of the ongoing star formation.  I present the early
evolution of DM-free models of dwarf galaxies in which star formation
efficiency, temperature threshold, initial distribution of gas and
infall are varied.  I conclude that it is feasible to keep a fraction
of gas bound for several hundreds of Myr and that the development of
galactic winds does not necessarily stop continuous star
formation. The evolution of metallicity of these models significantly
depend on the adopted star formation criteria. The evolution of
similar models with a large DM halo does not differ very substantially
from the evolution of DM-free models. This implies that, at least in the
first hundreds Myr, the global distribution of gas, more than the depth
of the potential well, affects the evolution of the dwarf galaxies and
the formation of large-scale outflows.