Multicolor CCD Photometry and Period Analysis of Three Pulsating Variable Stars
Kevin B. Alton
UnderOak Observatory, 70 Summit Avenue, Cedar Knolls, NJ 07927
Received November 21, 2013; revised January 14, 2014; accepted January 28, 2014
Multicolor CCD photometry of three pulsating variable stars, RR Leo, TYC 790-1124-1, and V337 Ori has lead to period solutions using Fourier methods on light curves acquired at UnderOak Observatory (UO). New photometric data from RR Leo largely corroborate findings previously reported for this well-studied RRab variable. An O–C diagram period analysis using a rich historical record of time-of-maximum light data produced an updated quadratic ephemeris for RR Leo. Although not compelling, underlying sinusoidal variability in the quadratic residuals suggest that this intrinsic variable may also have a gravitationally bound cohort. Light curves from the poorly studied HADS variable TYC 790-1124-1 were remarkably symmetrical; this behavior was observed during a single campaign in 2011 which lasted only one month. Fortunately, starting nearly a decade ago photometric data were also captured by the ASAS survey between 2002 and 2009; the combined results reveal that the fundamental period and light curve shape for TYC 790-1124-1 has substantively remained unchanged. V337 Ori has only been studied by two other investigative groups within the past three years; their results and the two most prominent pulsation frequencies at 4.96877 and 6.72 c/d detected in the UO light curves are in good agreement. Notably, this HADS exhibits significant cycle-to-cycle amplitude variability which may be related to these and other pulsation modes not detected in the present study.