Abstract
Using thee‐dimensional radiation hydrodynamics (RHD) simulations, we explore the radiative feedback process on the secondary Population III (Pop III) star formation. As recently shown by Umemura et al. (2010), a density peak can independently collapse in the distance of ∼60 pc from a precollapsed density peak. Since Pop III stars are expected to be very massive, strong UV radiation from a Pop III star born in a precollapsed density peak is likely to play a crucial role on the fate of an adjacent density peak. By RHD simulations, we find that the adjacent peak can survive although a shock associated with ionization front strips a large amount of gas. The surviving cloud is never ionized, but H2 molecule fraction is higher than that in usual Pop III cloud. Based on the obtained physical quantities of the cloud, we also discuss the mass of the secondary Pop III star.
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