AAS 205th Meeting, 9-13 January 2005
Session 54 Pulsating Stars: RR Lyraes, Miras, Cepheids, etc.
Poster, Tuesday, January 11, 2005, 9:20am-6:30pm, Exhibit Hall

Previous   |   Session 54   |   Next

[54.17] 53 Persei Observations, 14 Years of Persistence Rewarded

R. J. Dukes, Jr., L. R. Mills (Coll. Charleston)

We report the analysis of fourteen years of observations of the non-radially pulsating star, 53 Persei, obtained with the Four-College Consortium Automatic Photoelectric Telescope (APT). We previously discussed analyses of four (AAS 185th meeting, #80.07, 1994) and ten seasons (AAS 197th meeting, #46.11, 2000) respectively. In this paper we present a summary of the analysis of the entire fourteen seasons of data. 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 2004. Our analysis of these observations shows that the two frequencies (0.46 c d-1 and 0.59 c d-1) identified by Smith, et. al. (Ap. J. 282, 226, 1984) and confirmed by Huang, et. al. (Ap. J. 431, 850, 1994) are present. In addition to the four other frequencies we earlier reported we now extend our list to eleven frequencies. Five of these are apparently combination terms. The complete list is f1=0.4612 c d-1, f2=0.5939 c d-1, f3=0.4715 c d -1, f4=0.5689 c d-1, f5=0.2593 c d-1, f6=0.6636 c d-1, f1+f2=1.05517 c d -1, 2f5=0.5186 c d-1, f1+f4 =0.9328 c d-1, f1 +f2+f5 = 1.31 c d-1, and f4-2f5=0.05 c d-1. Some of the combination terms are stronger than some of the main frequencies. For terms of sufficient strength to permit adequate phase determination their position on the amplitude ratio versus phase difference plot for Stromgren photometry from the models of Townsend (MNRAS, 330, 855, 2002) indicate that these are all l =1, g-modes. Finally, the strongest frequencies show a significant (u-b) color variation. There is also some indication of either a frequency splitting in the strongest terms and/or a slight change in these frequencies over the fourteen years of observation. This work has been supported in part by NSF grants #AST86-16362, #AST91-15114, #AST95-28906, and #AST-0071260 to the College of Charleston.

If you would like more information about this abstract, please follow the link to www.cofc.edu/~dukesr/. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: dukesr@cofc.edu

Previous   |   Session 54   |   Next

Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.