  We report on extensive photometry of the dwarf nova SS Ursae Minoris
throughout nine months of 2004. In total, we recorded two superoutbursts and 11
normal outbursts of the star. SS UMi has been known to show frequent
superoutbursts with a mean interval of 84.7 days. Our data suggest that the
interval between successive superoutbursts lengthened to 197 days, indicating
that SS UMi entered a period of untypical behavior manifested by a growth in
the quiescent magnitude of the star and a series of frequent, low-amplitude,
normal outbursts observed from July to September 2004.
  The mean superhump period derived for the April 2004 superoutburst of SS UMi
is 0.070149(16) days (101.015 min). Combining this value with an earlier
orbital period determination, we were able to derive the period excess, which
is equal to 3.5 +/- 1.6%, and estimate the mass ratio of the binary system as
equal to q=0.16 +/- 0.07.
  During the entire superoutburst, the period decreased at a rate of $\dot
P/P_{\rm sh} = -6.3(1.4) \times 10^{-5}$. However, detailed analysis of the
timings of superhump maxima seem to suggest a more complex period change, with
a decrease in the period during the first and last stages of the superoutburst
but an increase in the middle interval.
