  Continuing the project described by Kato et al. (2009, PASJ 61, S395,
arXiv:0905.1757), we collected times of superhump maxima for 51 SU UMa-type
dwarf novae mainly observed during the 2010-2011 season. Although most of the
new data for systems with short superhump periods basically confirmed the
findings by Kato et al. (2009) and Kato et al. (2010, PASJ 62, 1525,
arXiv:1009.5444), the long-period system GX Cas showed an exceptionally large
positive period derivative. An analysis of public Kepler data of V344 Lyr and
V1504 Cyg yielded less striking stage transitions. In V344 Lyr, there was
prominent secondary component growing during the late stage of superoutbursts,
and the component persisted at least for two more cycles of successive normal
outbursts. We also investigated the superoutbursts of two conspicuous eclipsing
objects: HT Cas and the WZ Sge-type object SDSS J080434.20+510349.2. Strong
beat phenomena were detected in both objects, and late-stage superhumps in the
latter object had an almost constant luminosity during the repeated
rebrightenings. The WZ Sge-type object SDSS J133941.11+484727.5 showed a phase
reversal around the rapid fading from the superoutburst. The object showed a
prominent beat phenomenon even after the end of the superoutburst. A pilot
study of superhump amplitudes indicated that the amplitudes of superhumps are
strongly correlated with orbital periods, and the dependence on the inclination
is weak in systems with inclinations smaller than 80 deg.
