Ostriker and Gnedin  have carried out high resolution numerical simulations of the reheating and reionization of the Universe due to star formation bursts triggered by molecular hydrogen cooling. Accounting for the chemistry of the primeval hydrogen/helium plasma, self-shielding of the gas, radiative cooling, and a phenomenological model of star formation, they find that two distinct star populations form: the first generation pop III from cooling prior to reheating at redshift ; and the second generation pop II at z <10 when the virial temperature of the gas clumps reaches K and hydrogen line cooling becomes efficient. Star formation slows in the intermittent epoch due to the depletion of by photo-destruction and reheating. In addition, the objects which formed pop III stars also initiate pop II sequences when their virial temperatures reach K through continued mass accretion.
|Computational Cosmology: from the Early Universe to the
Large Scale Structure
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