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The Structure and Evolution of Early Cosmological HiiRegions
We study the formation and evolution of HII regions around the first stars formed at z=10-30. We use a one-dimensional Lagrangian hydrodynamics code which self-consistently incorporates radiative transfer and non-equilibrium primordial gas chemistry. The star-forming region is defined as a spherical gas cloud with a Population III star embedded at the center. We explore a large parameter space of host halo mass, gas density profile, and stellar luminosity. The formation of the HII region isdoi:10.1086/423313 fatcat:bgmicxzonbdwjeklnsq7sbvdne