Discovery of a new SU UMa-type dwarf nova, V 1028 Cygni

V-band high-speed CCD photometry of V 1028 Cyg revealed that hump structure s existed in the early stage of its 1995 July outburst. We obtained 0.06154 (+/-0.00002)d as the best estimated period of super-humps. We confirmed th at this dwarf nova belongs to the SU UMa stars. A re-brightening occurred a fter the superoutburst, and may be associated with a normal outburst. An an alysis of the timings of superhump axima showed clear evidence for an incre ase of the superhump period (P-dot = P/P) with 7.54 x 10(-6) Only a few sta rs (AL Com, T Leo, SW UMa, etc.) are reported to have such an increase of t he superhump period. At the end of the superoutburst, Ne detected that the amplitude of the superhumps increased considerably. Both of these propertie s are not typical features of ordinary SU UMa stars. The connection between the WZ Sge-type and the SU UMa-type dwarf novae is briefly discussed.