Lyman α Radiation Hydrodynamics of Galactic Winds Before Cosmic Reionization

Abstract

The dynamical impact of Lyman-alpha (Ly{\alpha}) radiation pressure on galaxy formation depends on the rate and duration of momentum transfer between Ly{\alpha} photons and neutral hydrogen gas. Although photon trapping has the potential to multiply the effective force, ionizing radiation from stellar sources may relieve the Ly{\alpha} pressure before appreciably affecting the kinematics of the host galaxy or efficiently coupling Ly{\alpha} photons to the outflow. We present self-consistent Ly{\alpha} radiation-hydrodynamics simulations of high-z galaxy environments by coupling the Cosmic Ly{\alpha} Transfer code (COLT) with spherically symmetric Lagrangian frame hydrodynamics. The accurate but computationally expensive Monte-Carlo radiative transfer calculations are feasible under the one-dimensional approximation. The initial starburst drives an expanding shell of gas from the centre and in certain cases Ly{\alpha} feedback significantly enhances the shell velocity. Radiative feedback alone is capable of ejecting baryons into the intergalactic medium (IGM) for protogalaxies with a virial mass of Mvir≲108 M⊙. We compare the Ly{\alpha} signatures of Population III stars with 105 K blackbody emission to that of direct collapse black holes with a nonthermal Compton-thick spectrum and find substantial differences if the Ly{\alpha} spectra are shaped by gas pushed by Ly{\alpha} radiation-driven winds. For both sources, the flux emerging from the galaxy is reprocessed by the IGM such that the observed Ly{\alpha} luminosity is reduced significantly and the time-averaged velocity offset of the Ly{\alpha} peak is shifted redward.