%0 Generic %1 Aykutalp2011 %A Aykutalp, Aycin %A Spaans, Marco %D 2011 %K low metal popIII uvb %T The complexity that the first stars brought to the Universe: Fragility of metal enriched gas in a radiation field %U http://arxiv.org/abs/1105.5158 %X The initial mass function of the first (Population III) stars and Population II (Pop II) stars is poorly known due to a lack of observations of the period between recombination and re-ionization. In simulations of the formation of the first stars, it has been shown that, due to the limited ability of metal-free primordial gas to cool, the IMF of the first stars is a few orders of magnitude more massive than the current IMF. The transition from a high-mass IMF of the first stars to a lower-mass current IMF is thus important to understand. To study the underlying physics of this transition, we performed several simulations using the cosmological hydrodynamical adaptive mesh refinement code Enzo for metallicities of 10^-4, 10^-3, 10^-2, 10^-1 Z_ødot. In our simulations we include a star formation prescription that is derived from a metallicity dependent multi-phase ISM structure, an external UV radiation field, and a mechanical feedback algorithm. We also implement cosmic ray heating, photoelectric heating and gas-dust heating/cooling, and follow the metal enrichment of the ISM. It is found that the interplay between metallicity and UV radiation leads to the co-existence of Pop III and Pop II star formation in non-zero metallicity (Z/Z_ødot \geq10^-2) gas. A cold (T<100 K) and dense (\rho>10^-22 g cm^-3) gas phase is fragile to ambient UV radiation. In a metal-poor (Z/Z_ødot łeq10^-3) gas, the cold and dense gas phase does not form in the presence of a radiation field of F_0\sim10^-5-10^-4 erg cm^-2 s^-1. Therefore, metallicity by itself is not a good indicator of the Pop III-Pop II transition. Metal-rich (Z/Z_ødot\geq10^-2) gas dynamically evolves two to three orders of magnitude faster than metal poor gas (Z/Z_ødotłeq10^-3). The simulations including SNe show that pre-enrichment of the halo does not affect the mixing of metals

@misc{Aykutalp2011, abstract = { The initial mass function of the first (Population III) stars and Population II (Pop II) stars is poorly known due to a lack of observations of the period between recombination and re-ionization. In simulations of the formation of the first stars, it has been shown that, due to the limited ability of metal-free primordial gas to cool, the IMF of the first stars is a few orders of magnitude more massive than the current IMF. The transition from a high-mass IMF of the first stars to a lower-mass current IMF is thus important to understand. To study the underlying physics of this transition, we performed several simulations using the cosmological hydrodynamical adaptive mesh refinement code Enzo for metallicities of 10^{-4}, 10^{-3}, 10^{-2}, 10^{-1} Z_{\odot}. In our simulations we include a star formation prescription that is derived from a metallicity dependent multi-phase ISM structure, an external UV radiation field, and a mechanical feedback algorithm. We also implement cosmic ray heating, photoelectric heating and gas-dust heating/cooling, and follow the metal enrichment of the ISM. It is found that the interplay between metallicity and UV radiation leads to the co-existence of Pop III and Pop II star formation in non-zero metallicity (Z/Z_{\odot} \geq10^{-2}) gas. A cold (T<100 K) and dense (\rho>10^{-22} g cm^{-3}) gas phase is fragile to ambient UV radiation. In a metal-poor (Z/Z_{\odot} \leq10^{-3}) gas, the cold and dense gas phase does not form in the presence of a radiation field of F_{0}\sim10^{-5}-10^{-4} erg cm^{-2} s^{-1}. Therefore, metallicity by itself is not a good indicator of the Pop III-Pop II transition. Metal-rich (Z/Z_{\odot}\geq10^{-2}) gas dynamically evolves two to three orders of magnitude faster than metal poor gas (Z/Z_{\odot}\leq10^{-3}). The simulations including SNe show that pre-enrichment of the halo does not affect the mixing of metals }, added-at = {2011-05-27T18:31:56.000+0200}, author = {Aykutalp, Aycin and Spaans, Marco}, biburl = {https://www.bibsonomy.org/bibtex/256ccd27ca4d847dadae8ac8c01dd1828/miki}, description = {[1105.5158] The complexity that the first stars brought to the Universe: Fragility of metal enriched gas in a radiation field}, interhash = {9e25c918a9c96e081ae1314386fff51c}, intrahash = {56ccd27ca4d847dadae8ac8c01dd1828}, keywords = {low metal popIII uvb}, note = {cite arxiv:1105.5158 Comment: 20 pages, 16 figures, accepted to ApJ}, timestamp = {2011-05-27T18:31:56.000+0200}, title = {The complexity that the first stars brought to the Universe: Fragility of metal enriched gas in a radiation field}, url = {http://arxiv.org/abs/1105.5158}, year = 2011 }