Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 453, Issue 1, Pages 277-286Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv1589
Keywords
stars: early-type; stars: oscillations; stars: rotation
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Funding
- Polish NCN [DEC-2012/05/N/ST9/03905, 2011/01/M/ST9/05914, 2011/01/B/ST9/05448]
- Wroclaw Centre for Networking and Supercomputing [265]
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Interpretation of the oscillation spectrum of the slowly pulsating B-type (SPB) star HD 21071 is presented. We show that non-rotating models cannot account for the two highest amplitude frequencies and taking into account the effects of rotation is necessary. Rotating seismic models are constructed using various chemical compositions, opacity data, core overshooting parameters and rotational velocities. There are prospects for seismic modelling of SPB stars, even if no asymptotic pattern is observed in their oscillation spectra, provided an unambiguous mode identification is doable and the effects of rotation are properly included.
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