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| Paper: |
New Beta Cephei Suspect in the chi Persei Cluster |
| Volume: |
135, A Half Century of Stellar Pulsation Interpretations: a Tribute to Arthur N. Cox |
| Page: |
157 |
| Authors: |
Krzesinski, J. |
| Abstract: |
We have shown recently (Krzesinski 1995, Krzesinski and Pigulski 1997) that the b Cephei-type variables are present in the open clusters h and chi Persei. CCD observations made in 1994 and 1996 at Mt. Suhora Observatory uncovered three such stars in central regions of these clusters (Oo 692 ** in h Per and Oo 2299 and Oo 2246 in chi Per). In this report we present the new CCD observations of h and chi Per, carried out during fall of 1996 and at the beginning of 1997. The most promising new b Cephei candidate, Oo 2444, (B=9.83, B-V = +0.32) shows low amplitude variations (~0.006 mag.) with a period of approximatelly 0.17 days. The star is very close to the instability strip determined by the two b Cephei-type stars found previously in this cluster. The variability is clearly visible during one night, but is undetectable during the other night. Such a behaviour is not uncommon among the b Cephei-type stars and might be due to beating of closely spaced frequencies. Our current dataset is as yet too short for a reliable determinations of the periods (and amplitudes) of the modes involved - if the star pulsates. ** Oo - means Oosterhoff numbers (Oosterhoff 1937). References: Krzesinski J. 1995, ASP Conf. Ser. 83, 299 Krzesinski J. and Pigulski A. 1997, Astron. Astroph. in press Oosterhoff P.Th. 1937, Ann. Sterre. Leiden, 17, 5 |
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