Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.2910t&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #29.10; Bulletin of the American Astronomical Society, V
Astronomy and Astrophysics
Astronomy
Scientific paper
In 1996 an analysis of Hipparcos observations revealed that the star HD 32456 was a Cepheid variable with a period of 3.29 days. Further photometric observations confirmed this and enabled the period to be refined to 3.2942 days. An inspection of the photometric light curves show relatively small scatter indicating that this is a singly periodic Cepheid. However, since approximately 10% of Cepheids with periods less than 5 days are double mode and there are only 22 double mode Cepheids known it seems important to verify this. We therefore decided to place this star on the observing program of the Four College Consortium Automatic Photometric Telescope in order to investigate the possible presence of a secondary period. During the 1998 observing season we obtained 274 Stromgren uvby observations of this star spread over one hundred days. A preliminary analysis of the data revealed that it was one of the shortest period fundamental mode Cepheids with a slight indication of a second period with a value close to that expected for a first overtone. Therefore additional 526 observations were obtained during the 2005-2006 observing seasons. Combining all observations gave no indication of a first overtone term. Separate analysis of the two sets of data yielded slightly different frequencies with a 1996 value of 0.30348 c d-1 and a 2006 value of 0.30351 c d-1 . The latter is essentially identical to that from the combined data set as well as that of the archival study of Berdnikov et al. (IBVS, 4375, 1996). The question therefore is whether or not there is a relatively short term period variation. Observations are continuing in an attempt to answer this question. This work has been supported by a NSF Grants AST95-28906 and AST05-07551.
Dukes Robert J. Jr.
Taylor William Z.
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