Volume 432, Number 3, March IV 2005
|Page(s)||1013 - 1024|
|Section||Stellar structure and evolution|
|Published online||07 March 2005|
A study of bright southern slowly pulsating B stars*
III. Mode identification for singly-periodic targets in spectroscopy
Royal Observatory of Belgium, Ringlaan 3, 1180 Brussel, Belgium e-mail: email@example.com
2 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium
3 Astronomical Institute of the Wroclaw University, ul. Kopernika 11, 51-622 Wroclaw, Poland
4 Instituto de Astrofísica de Andalucía, CSIC, Apdo. 3004, 18080 Granada, Spain
5 Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du Six Août 17, 4000 Liège, Belgium
6 Department of Astrophysics, University of Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
Accepted: 30 November 2004
We present the results of the mode identification for a sample of 7 bright southern slowly pulsating B stars showing one pulsation frequency in the 413 nm Si II profiles. We combined the results from (1) the method of photometric amplitudes; (2) the moment method; and (3) the amplitude and phase variation across the profile to search for the and m values of the modes best fitting the data. It is the first time that the applicability of these techniques is tested to a sample of main-sequence g-mode pulsators. Combining the moment method with the amplitude and phase variations across the observed line profile gives an improvement in spectroscopic identification of low degree g-mode pulsations. Using the variations of the higher order even moments and of the moment method solutions can also help. For HD 181558, HD 24587, HD 140873 and HD 177863, the photometric and spectroscopic results are compatible and point towards = (1, +1) sectoral modes. For HD 215573, HD 53921 and HD 92287, the results are inconclusive. Our proposed methodology for mode identification is also applicable to γ Doradus stars.
Key words: stars: early-type / stars: variables: general / stars: oscillations / line: profiles
© ESO, 2005
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