We report time-resolved CCD photometry of the cataclysmic variable EG Aquarii during the 2006 November outburst During the outburst , superhumps were unambiguously detected with a mean period of 0.078828 ( 6 ) days , firstly classifying the object as an SU UMa-type dwarf nova .
It also turned out that the outburst contained a precursor .
At the end of the precursor , immature profiles of humps were observed .
By a phase analysis of these humps , we interpreted the features as superhumps .
This is the second example that the superhumps were shown during a precursor .
Near the maximum stage of the outburst , we discovered an abrupt shift of the superhump period by { \sim } 0.002 days .
After the supermaximum , the superhump period decreased at the rate of \dot { P } / P = - 8.2 { \times } 10 ^ { -5 } , which is typical for SU UMa-type dwarf novae .
Although the outburst light curve was characteristic of SU UMa-type dwarf novae , long-term monitoring of the variable shows no outbursts over the past decade .
We note on the basic properties of long period and inactive SU UMa-type dwarf novae .