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PU CMa superhump period Dear Colleagues, We have received new data from Peter Nelson. The data also clearly recorded superhumps. Combined with Monard's data, we have yielded a superhump period of 0.05832(5) d. This period is 2.9% longer than the orbital period. Because of the short visibilty in the evening sky, the period identification still needs to be confirmed by additional nights' observation. If this is the true superhump period, the fractional superhump excess of 2.9% is somewhat large for this period. The mean profile is posted at: http://vsnet.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/PU_CMa/push.gif The full amplitude is smaller than long-period SU UMa-type dwar novae. This may be a result of systematic decrease of the superhump amplitudes in shorter period systems, or the observations may have covered the epoch when the superhumps had started to decay. In any case, further observations (hopefully 2hr continuous run each night) are strongly encouraged! Regards, Taichi Kato VSNET Collaboration team
Return to the Daisaku Nogami
vsnet-adm@kusastro.kyoto-u.ac.jp
