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Session 26 - Stars in the Visible & IR.
Display session, Tuesday, June 10
South Main Hall,
The non-radially pulsating star, 53 Persei, has been observed for the last six years by the Four-College Consortium Automatic Photoelectric Telescope (APT) on Mt. Hopkins. After elimination of observations not passing the various observational checks which have been devised to eliminate APT observations obtained under non-photometric conditions, we have approximately 1000 observations acquired on 366 nights from the Fall of 1990 through the Spring of 1996. 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, 26, 1447, 1994) now appears to be a close doublet. There is at least one other term present in all six seasons (0.51 c/d) as well as a coupling term between the two strongest (1.05 c/d). Finally, the strongest frequencies show a significant (u-b) color variation. The work has been supported in part by NSF grants AST86-16362, AST91-15114, USE91056184, and AST95-28506 to the College of Charleston.
