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Density inhomogeneity in the intergalactic medium (IGM) can boost therecombination rate of ionized gas substantially, affecting the growth of HIIregions during reionization. Previous attempts to quantify this effecttypically failed to resolve down to the Jeans scale in the pre-ionization IGM,which is important in establishing this effect, along with the hydrodynamicalback-reaction of reionization on it. Towards that end, we perform a set offully-coupled, radiation-hydrodynamics simulations from cosmological initialconditions, extending the mass resolution of previous work to the scale ofminihalos. Pre-reionization structure is evolved until a redshift $z_i$ atwhich the ionizing radiation from external sources arrives to sweep an R-typeionization front supersonically across the volume in a few Myr, until it istrapped on the surfaces of minihalos and converted to D-type, after which theminihalo gas is removed by photoevaporative winds. Small-scale densitystructures during this time lead to a high ($>$10) clumping factor for ionizedgas, which hugely boosts the recombination rate until the structures aredisrupted by the hydrodynamic feedback after $\sim 10-100~\rm{Myr}$. Forincoming stellar radiation with intensity $J_{21}$ in a $200~h^{-1}~\rm{kpc}$box with the mean density contrast $\bar\delta$, the number of extrarecombinations per H atom, on top of what is expected from homogeneouslydistributed gas, is given by$0.32[J_{21}]^{0.12}[(1+z_i)/11]^{-1.7}[1+\bar\delta]^{2.5}$. In models inwhich most of the volume is ionized toward the end of reionization, this canadd more than one recombination per H atom to the ionizing photon budget toachieve reionization.

The Hydrodynamic Feedback of Cosmic Reionization on Small-Scale Structures and Its Impact on Photon Consumption during the Epoch of Reionization