Lyman–Werner UV escape fractions from primordial haloes

摘要: Population III stars can regulate star formation in the primordial Universe several ways. They ionize nearby halos, and even if their ionizing photons are trapped by own Lyman-Werner (LW) still escape destroy H$_2$ other preventing them from cooling forming stars. LW fractions thus a key parameter cosmological simulations of early reionization but have not yet been parametrized for realistic halos halo or stellar mass. To do so, we perform radiation hydrodynamical UV 9--120 M$_{\odot}$ Pop $10^5$ to $10^7$ with ZEUS-MP. We find that lines (i.e. those responsible destroying H$_{2}$ systems) ranging 0% 85%. No most massive our sample, star. Escape elsewhere 11.18--13.6~eV energy range, which be redshifted into at distances, generally much higher, being above 60% all least halos. shielding neutral hydrogen, has neglected studies date, produces up factor three smaller than predicted self-shielding alone.