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The apparition of the first stars radically changed the state of the gas in the Univers.  With their highly energetic radiation, they heat up and ionize the surrounding gas.  Moreover, at the end of their life, stars explode in supernovae, which create swirl in the gas around them.  But this gas is also the main material use to grow the next generation of stars, and a change in his state could have consequence on the star formation rate (hereafter SFR)  of the futures generations. To study this period of intense change, induced by a complex coupling into different physics, we need to use numerical simulations.