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First Stars III
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Poster
Title: The evolution of supernovae remnants in the early universe Author(s): Takanori Nagakura Abstract: We investigate the evolution of supernova remnants in the early universe using one-dimensional hydrodynamics with spherical symmetry along with non-equilibrium chemistry. A cooled dense shell, which is formed behind the supernova blastwave during snowplough phase, is thought to be important site where the next generation of stars are born. To elucidate characteristic fragment mass of the shell, we calculate its thermal and chemical evolution in detail. We show that the shell cools through H$_2$ or HD line cooling in the case of the metal-free or extremely low-metallicity environments($Z \le 10^{-4} Z_{\odot}$), while that the fine-structure line of carbon and oxygen dominates the coolings of the shell for more metal abundant enviroments($Z \ge 10^{-3} Z_{\odot}$). However, the minimum temperature of the shell is limited by the cosmic microwave background radiation, which leads that the temperature of the shell is less dependent on the metallicity of the gas in our simulated density ranges. The linear stability analysis on the shell coupled with our results suggests that the fragmentation of the shell will strongly depend on the number density of the ambient medium and the supernovae energy but little depend on the metallicity of the gas.
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