Metal enrichment of the primordial interstellar medium through three-dimensional hydrodynamical evolution of the first supernova remnant

The long-term evolution of supernova (SN) remnants in the primordial inters tellar medium (ISM) with an inhomogeneous structure is calculated to invest igate metal enrichment of the primordial gas. For this purpose, we have con structed a parallel three-dimensional hydrodynamics code incorporating the radiative cooling and self-gravity. The self-gravity and radiative cooling develop the inhomogeneous structure of the ISM from a small perturbation wi th a power-law spectrum. The resultant density ranges from 0.5 to 10(6) cm( -3). Calculations for an SN with the progenitor mass of 20 M-circle dot are performed as the first step of a series of our study. It is found from the results that a single SN distributes some of the newly synthesized heavy e lements into a dense filament of the ISM with densities ranging from 100 to 10(4) cm(-3) depending on where the SN explodes. Thus, the metallicity [Mg /H] of the dense filaments polluted by the SN ejecta becomes -2.7 +/- 0.5. From these filaments, the first Population LI stars will form. This value i s in accordance with previous analytical work by Shigeyama & Tsujimoto with an accuracy of similar to 0.3 dex.