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We analyze the cycles in the possible intermediate polar V795 Her, the optical counterpart of 2RXP J171256.0+333121, using the photometric V band CCD observations obtained within 5 days in 2008. We find that the times of the minimum intensity of the known cycle of ∼2.8028 hours are more stable than those of the peak intensity. We show that while the smoothed profile of the folded intensity curve is single‐peaked, the profile of its residuals is double‐peaked. We resolve the variations of the superimposed cycle of ∼0.01 d during a single night; this cycle is thus not caused by spin modulation of the white dwarf. We discuss our observations in terms of superhumps.