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Asteroseismology with the new opacity bump at log T ≈ 5.06

Published online by Cambridge University Press:  18 February 2014

H. Cugier
H. Cugier*
Affiliation:
Astronomical Institute of the Wroclaw University, 51-622 Wroclaw, Poland, email: [email protected]
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Abstract

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Although the κ mechanism of pulsations is known for early-type stars, opacities and the equation of state are still uncertain. Stellar models calculated for the OP data implemented with the new Kurucz opacities at log T < 5.2 were investigated for different chemical compositions of elements. The additional metallic opacity bump at log T ≈ 5.06 that occurs in the Kurucz data changes markedly the oscillation spectra of unstable modes. Basic properties of the new opacity bump and examples of seismic models are shown. B-type stars observed in the Galaxy, LMC and SMC were considered. The problem was studied using Dziembowski's computing codes for linear, non-adiabatic and non-radial oscillations.

Keywords

starsstellar evolutionasteroseismologyradiative opacity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 401 - 402
Copyright
Copyright © International Astronomical Union 2014 

References

Castelli, F. & Kurucz, R. 2003, in: Piskunov, N., Weiss, W. W., & Gray, D. F. (eds.), Modelling of Stellar Atmospheres, Proc. IAU Symposium No. 210 (Astronomical Society of the Pacific), Poster A20Google Scholar
Cugier, H. 2012, A&A, 547, 42Google Scholar
Dziembowski, W. 2009, CoAst, 158, 227Google Scholar
Kurucz, R. 2011, Can. J. Phys., 89, 417CrossRefGoogle Scholar
Pamyatnykh, A. A. 1999, AcA, 49, 119Google Scholar
Pradhan, A. K. & Nahar, S. N. 2009, AIP-CP, 1171, 52Google Scholar
Seaton, M. J., Yan, Y, Mihalas, D., & Pradhan, A. K. 1994, MNRAS, 266, 805Google Scholar