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Supernova explosions and their remnants (SNRs) drive important feedbackmechanisms that impact considerably the galaxies that host them. Then, theknowledge of the SNRs evolution is of paramount importance in the understandingof the structure of the interstellar medium (ISM) and the formation andevolution of galaxies. Here we study the evolution of SNRs in homogeneousambient media from the initial, ejecta-dominated phase, to the final,momentum-dominated stage. The numerical model is based on the Thin-Shellapproximation and takes into account the configuration of the ejected gas andradiative cooling. It accurately reproduces well known analytic and numericalresults and allows one to study the SNR evolution in ambient media with a widerange of densities $n_{0}$. It is shown that in the high density cases, strongradiative cooling alters noticeably the shock dynamics and inhibits theSedov-Taylor stage, thus limiting significantly the feedback that SNRs provideto such environments. For $n_{0}>5 \times 10^{5}$ cm$^{-3}$, the reverse shockdoes not reach the center of the explosion due to the rapid fall of the thermalpressure in the shocked gas caused by strong radiative cooling.

The full evolution of supernova remnants in low and high density ambient media