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Hube and Aikman (PASP, 103, 49, 1991) reported the star 3 Vulpeculae was both a spectroscopic binary and a possible member of the 53 Persei class of variables. The latter determination was made on the basis of Silicon II line profile variations; although, a limited amount of photometry also suggested a night-to-night brightness variation. Since brightness variation due to non-radial pulsation is one of the characteristics of the 53 Persei stars, we placed this star on the observing program of the College's automatic photoelectric telescope. In this paper we report on photometric observations obtained during the 1991 through 1994 observing seasons in the Stromgren uvby photometric system. Periodogram analysis shows both the 1.03 day period (similar to that found in the line profile variation by Hube and Aikman) as well as a weaker 1.26 day variation. This work has been supported in part by NSF grants AST86-16362, AST91-15114, and USE-9156184 to the College of Charleston.
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