On the theory of mass loss in dwarf galaxies: I - basic equations and
  the case of wave/thermal driven winds
  In this work we present a semi-analytical model of galactic wind for dwarf
galaxies where thermal and turbulent/momemtum driving mechanisms are studied.
The model takes into account wave and internal adiabatic heating mechanisms, as
well as radiative and adiabatic cooling. The importance of external sources of
energy is discussed. We also studied the role of the spatial distribution of
dark matter in the acceleration of the wind and on the mass loss rates. The
basic model parameters that regulate the wind mass loss rate and terminal
velocity are the gravitational potential profile, the equilibrium temperature
of the gas and the amplitude of the turbulent motions of the gas. We found that
dwarf galaxies are likely to present quasi-stationary winds with mass loss
rates larger than $10^{-3}$M$_{\odot}$yr$^{-1}$ even in the absence of
turbulent motions (which is possibly related to the SNe feedback), if the
interstellar gas is heated to $T > 10^4 - 10^5$K. We also found that the wind
mass loss rate is enhanced for cusped dark matter distributions, such as the
NFW-profile, due to the increased pressure gradients at the center of the
galaxy. The solutions presented here may serve as benchmarks for numerical
simulations, and as inputs for single zone chemical evolution models of dwarf
galaxies.
