2006CBET..736....1M

Further to CBET 734, G. Masi (Ceccano, Italy) provides details regarding his photometric observations of superhumps seen in this variable star. On Nov. 8.84 UT, a few hours after the outburst of EG Aqr was announced by R. Stubbings, Masi performed unfiltered, time-series photometry with the 28-cm f/5 "Virtual Telescope" at Ceccano. Real-time data reduction from the 60-s exposures showed the clear signature of superhumps with amplitude just under 0.1 magnitude (peak-to-peak), revealing the SU UMa-type nature of this cataclysmic variable (CV); a very quick check revealed an estimated superhump period close to 2 hours, near the lower limit of the CV period gap. During the 3-hr observation arc, the star faded by about 0.15 mag (the star was about 30 deg above the horizon, but the comparison stars showed no fading). On Nov. 9.73, the variable was observed again with the same equipment and found to be 0.3 mag brighter; superhumps had amplitude 0.35 mag, and an evaluation (performed using the Phase-Dispersion Minimization method during the 4-hr observation arc) revealed an estimated period of 1.99 hr. On Nov. 10.73, a 5-hr observation arc showed EG Aqr to be marginally fainter than on the previous night; the superhumps showed a different profile, with a full amplitude of 0.3 mag, with the superhump period evidently having shortened to 1.89 hr. As an attempt to combine the Nov. 9 and 10 data provides inadequate results, the shortening of the period appears to be real. (Using both the Nov. 9 and 10 data, a mean superhump period of 1.904 hr is obtained.)