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As is usual in dwarf spheroidal galaxies, today the Local Group galaxy UrsaMinor is depleted of its gas content. How this galaxy lost its gas is still amatter of debate. To study the history of gas loss in Ursa Minor, we conductedthe first three-dimensional hydrodynamical simulations of this object, assumingthat the gas loss was driven by galactic winds powered only by type IIsupernovae (SNe II). The initial gas setup and supernova (SN) rates used in oursimulations are mainly constrained by the inferred star formation history andthe observed velocity dispersion of Ursa Minor. After 3 Gyr of evolution, wefound that the gas removal efficiency is higher when the SN rate is increased,and also when the initial mean gas density is lowered. The derived mass-lossrates are systematically higher in the central regions (<300 pc), even thoughsuch a relationship has not been strictly linear in time and in terms of thegalactic radius. The filamentary structures induced by Rayleigh-Taylorinstabilities and the concentric shells related to the acoustic waves driven bySNe can account for the inferred mass losses from the simulations. Our resultssuggest that SNe II are able to transfer most of the gas from the centralregion outward to the galactic halo. However, other physical mechanisms must beconsidered in order to completely remove the gas at larger radii.

Three-dimensional hydrodynamical simulations of the supernovae-driven gas loss in the dwarf spheroidal galaxy Ursa Minor