Minihalo photoevaporation during cosmic reionization: evaporation times and photon consumption rates

Abstract

The weak, R-type ionization fronts (I-fronts) which swept across the intergalactic medium (IGM) during the reionization of the universe often found their paths blocked by cosmological minihaloes. When this happened, the neutral gas which filled each minihalo was photoevaporated; as the I-front burned its way through the halo, decelerating from R-type to D-type, all the gas was blown back into the IGM as an ionized, supersonic wind. In a previous paper (Shapiro, Iliev and Raga 2004), we described this process and presented our results of the first simulations of it by numerical gas dynamics with radiation transport in detail. For illustration we focused on the particular case of a 10^7 solar masses minihalo overrun at z=9 by an intergalactic I-front caused by a distant source of ionizing radiation, for different source spectra (either stellar from massive Pop. II or III stars, or QSO-like) and a flux level typical of that expected during reionization. In a LambdaCDM universe, minihaloes formed in abundance before and during reionization and, thus, their photoevaporation is an important, possibly dominant, feature of reionization, which slowed it down and wasted ionizing photons. We have now performed a larger set of high-resolution simulations to determine and quantify the dependence of minihalo photoevaporation times and photon consumption rates on halo mass, redshift, ionizing flux level and spectrum. We find that the average number of ionizing photons each minihalo atom absorbs during its photoevaporation is typically in the range 2-10. For the collapsed fraction in minihaloes expected during reionization, this can add about 1 photon per total atom to the requirements for completing reionization, potentially doubling the minimum number of photons required to reionize the universe.

arXiv comment11 pages, 6 figures, submitted to MNRAS

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