2009/12/31 by Daniel J. Whalen, Daniel Whalen, Robert M. Hueckstaedt +2 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Gamma-ray bursts and supernovae #Halo #Hypernova #Radiative transfer #Redshift #Reionization #Star formation #Stars #Stellar, planetary, and galactic studies #Supernova #astro-ph.CO
paper · pdf · doi:10.1088/0004-637x/712/1/101
published as Astrophys.J.712:101-111,2010 · 13 pages, 11 figures, accepted by ApJ
arxiv created 2010/01/15 · openalex publication_date 2010/02/24 · arxiv updated 2014/11/20 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Ionizing UV radiation and supernova (SN) flows amidst clustered minihalos at high redshift regulated the rise of the first stellar populations in the universe. Previous studies have addressed the effects of very massive primordial stars on the collapse of nearby halos into new stars, but the absence of the odd–even nucleosynthetic signature of pair-instability SNe in ancient metal-poor stars suggests that Population III stars may have been less than 100 M ☉ . We extend our earlier survey of local UV feedback on star formation to 25–80 M ☉ stars and include kinetic feedback by SNe for 25–40 M ☉ stars. We find radiative feedback to be relatively uniform over this mass range, primarily because the larger fluxes of more massive stars are offset by their shorter lifetimes. Our models demonstrate that prior to the rise of global UV backgrounds, Lyman–Werner (LW) photons from nearby stars cannot prevent halos from forming new stars. These calculations also reveal that violent dynamical instabilities can erupt in the UV radiation front enveloping a primordial halo, but that they ultimately have no effect on the formation of a star. Finally, our simulations suggest that relic H ii regions surrounding partially evaporated halos may expel LW backgrounds at lower redshifts, allowing stars to form that were previously suppressed. We provide fits to radiative and kinetic feedback on star formation for use in both semianalytic models and numerical simulations.