Volume 456, Number 1, September II 2006
|Page(s)||261 - 268|
|Section||Stellar structure and evolution|
|Published online||23 August 2006|
Asteroseismology of the new multiperiodic γ Dor variable HD 239276
Instituto de Astrofísica de Andalucía, CSIC, PO Box 3004, 18080 Granada, Spain e-mail: firstname.lastname@example.org
2 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China
3 CRAAG, Algiers Observatory, BP 63 Bouzareah 16340, Algiers, Algeria
4 LESIA, Observatoire de Paris-Meudon, UMR 8109, 92190 Meudon, France
Accepted: 10 May 2006
The variability of HD 239276 was suspected photometrically nearly twenty years ago, but was confirmed with new observations obtained in 2001 during a two-site photometric campaign carried out from Spain, in uvbyβ Strömgren-Crawford photometry, and China, using the Johnson V filter. Two low-dispersion spectra were also collected. The results establish this star as a new multiperiodic γ Dor-type pulsator with deficiency in metallicity. Its possible λ Boo nature is discussed. The frequency analysis shows three pulsational frequencies as significant, but some more are probably present among the residuals. The method based on phase shifts and amplitude ratios in multicolour photometry is used to identify the excited modes with non-adiabatic time-dependent convection models. A very good agreement between the theoretical and observed amplitude ratios is obtained and the two main modes are identified as modes. Nevertheless, our results do not allow us to discriminate between a solar abundance and a metal deficient nature for this star. The frequency ratio method is further used for the identification of the modes. The results suggest low metallicity for this star, but a λ Boo nature may be not ruled out.
Key words: stars: variables: general / stars: individual: HD 239276 / stars: oscillations / techniques: photometric
© ESO, 2006
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