Abstract
The dwarf spheroidal (dSph) galaxy Ursa Minor shares a same characteristic found in other classical dSph galaxies in the Local Group: a low amount of gas inferred nowadays. Using non-cosmological, three-dimensional hydrodynamical simulations, we analyzed the impact of supernovae blasts on an initial isothermal gas configuration in hydrostatic equilibrium with a cored dark matter gravitational potential suitable for the Ursa Minor galaxy. Our results indicates that supernovae can remove more than a half of the initial gas mass inside the tidal radius of Ursa Minor after 3 Gyr of evolution (the estimated duration of the star formation episodes in Ursa Minor).
