  During the epoch of reionization, local variations in the ionized fraction
(patchiness) imprint arcminute-scale temperature anisotropies in the CMB
through the kinetic Sunyaev-Zel'dovich (kSZ) effect. We employ an improved
version of an analytic model of reionization devised in Furlanetto et al.(2004)
to calculate the kSZ anisotropy from patchy reionization. This model uses
extended Press-Schechter theory to determine the distribution and evolution of
HII bubbles and produces qualitatively similar reionization histories to those
seen in recent numerical simulations. We find that the angular power spectrum
of the kSZ anisotropies depends strongly on the size distribution of the HII
bubbles and on the duration of reionization. In addition, we show that upcoming
measurements of the kSZ effect should be able to distinguish between several
popular reionization scenarios. In particular, the amplitude of the patchy
power spectrum for reionization scenarios in which the IGM is significantly
ionized by Population III stars (or by mini-quasars/decaying particles) can be
larger (or smaller) by over a factor of 3 than the amplitude in more
traditional reionization histories (with temperature anisotropies that range
between 0.5 and 3 micro-Kelvin at l = 5000). We highlight the differences in
the kSZ signal between many possible reionization morphologies and discuss the
constraints that future observations of the kSZ will place on this epoch.
