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We present the study of a set of N-body+SPH simulations of a Milky Way-likesystem produced by the radiative cooling of hot gas embedded in a dark matterhalo. The galaxy and its gaseous halo evolve for 10 Gyr in isolation, whichallows us to study how internal processes affect the evolution of the system.We show how the morphology, the kinematics and the evolution of the galaxy areaffected by the input supernova feedback energy E$_{\rm SN}$, and we compareits properties with those of the Milky Way. Different values of E$_{\rm SN}$ donot significantly affect the star formation history of the system, but the discof cold gas gets thicker and more turbulent as feedback increases. Our mainresult is that, for the highest value of E$_{\rm SN}$ considered, the galaxyshows a prominent layer of extra-planar cold (log(T)<4.3) gas extended up to afew kpc above the disc at column densities of $10^{19}$ cm$^{-2}$. Thekinematics of this material is in agreement with that inferred for the HI halosof our Galaxy and NGC 891, although its mass is lower. Also, the location, thekinematics and the typical column densities of the hot (5.3<log(T)<5.7) gas arein good agreement with those determined from the O$_{\rm VI}$ absorptionsystems in the halo of the Milky Way and external galaxies. In contrast withthe observations, however, gas at log(T)<5.3 is lacking in the circumgalacticregion of our systems.

The effect of stellar feedback on a Milky Way-like galaxy and its gaseous halo