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R. J. Dukes, L. R. Mills (Coll. Charleston)
The non-radially pulsating star, 53 Persei, has been observed for the last ten years by the Four-College Consortium Automatic Photoelectric Telescope (APT). During the first six seasons the telescope was located on Mt. Hopkins in southern Arizona. For the last four seasons it has been at the Fairborn Observatory in Washington Camp, Arizona. In this paper we present a comparison of our analysis of the first six years of data with a separate analysis of the last four years. We have eliminated observations not passing various observational checks that have been devised to eliminate APT observations obtained under non-photometric conditions. Our current data set runs from the Fall of 1990 through the Spring of 2000. Our analysis of these observations shows that the two frequencies (0.46 c/d and 0.59 c/d) identified by Smith, et. al. (Ap. J. 282, 226, 1984) and confirmed by Huang, et. al. (Ap. J. 431, 850, 1994) are present. The additional frequency at 0.47 c/d which we earlier reported (BAAS, 190, #26.04. 1997) to be a close doublet appears to be a single term in the latter set. We find another three frequencies ( 0.57 c/d, 1.055 c/d, and 0.52 c/d) present in both essentially independent data sets. We note that the 1.05 term is the sum of the two strongest terms. Finally, the strongest frequencies show a significant (u-b) color variation. This work has been supported in part by NSF grants #AST86-16362, #AST91-15114, #AST95-28906, and #AST-0071260 to the College of Charleston.
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