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We calculate the angular power spectrum of the Cosmic Microwave Background(CMB) temperature fluctuations induced by the kinetic Sunyaev-Zel'dovich (kSZ)effect from the epoch of reionization (EOR). We use detailed N-body+radiativetransfer simulations to follow inhomogeneous reionization of the intergalacticmedium (IGM). For the first time we take into account the "self-regulation" ofreionization: star formation in low-mass dwarf galaxies (10^8 M_\sun \lesssim M\lesssim 10^9 M_\sun) or minihalos (10^5 M_\sun \lesssim M \lesssim 10^8M_\sun) is suppressed if these halos form in the regions that were alreadyionized or Lyman-Werner dissociated. Some previous work suggested that theamplitude of the kSZ power spectrum from the EOR can be described by atwo-parameter family: the epoch of half ionization and the duration ofreionization. However, we argue that this picture applies only to simple formsof the reionization history which are roughly symmetric about thehalf-ionization epoch. In self-regulated reionization, the universe begins tobe ionized early, maintains a low level of ionization for an extended period,and then finishes reionization as soon as high-mass atomically-cooling halosdominate. While inclusion of self-regulation affects the amplitude of the kSZpower spectrum only modestly (\sim 10 %), it can change the duration ofreionization by a factor of more than two. We conclude that the simpletwo-parameter family does not capture the effect of a physical, yet complex,reionization history caused by self-regulation. When added to thepost-reionization kSZ contribution, our prediction for the total kSZ powerspectrum is below the current upper bound from the South Pole Telescope.Therefore, the current upper bound on the kSZ effect from the EOR is consistentwith our understanding of the physics of reionization.

The Kinetic Sunyaev-Zel'dovich effect as a probe of the physics of cosmic reionization: the effect of self-regulated reionization