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The chemical composition of β Cephei and hybrid pulsators in the solar neighbourhood

Published online by Cambridge University Press:  27 October 2016

Norbert Przybilla  and
Maria-Fernanda Nieva
Norbert Przybilla
Affiliation:
Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstr. 25/8, A-6020 Innsbruck, Austria email: norbert.przybilla@uibk.ac.at, maria-fernanda.nieva@uibk.ac.at
Maria-Fernanda Nieva
Affiliation:
Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstr. 25/8, A-6020 Innsbruck, Austria email: norbert.przybilla@uibk.ac.at, maria-fernanda.nieva@uibk.ac.at
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Abstract

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β Cephei variables are the most prominent pulsators among the massive stars on the upper main sequence, extending into the class of the rare hybrid β Cephei-SPB pulsators in the overlap region with the instability strip of the Slowly Pulsating B-stars. While the κ-mechanism has been identified as the driver of the pulsations, a comprehensive explanation of the excitation of the observed p- and g-modes is still lacking. In particular, the instability regions for these main-sequence B-type pulsators are still not fully consistent with any current opacity calculations. We have determined tight observational constraints on the chemical composition of a sample of β Cephei and hybrid pulsators in the solar neighbourhood, covering all elements with abundances log (X/H) + 12 > 7.3. The star sample turns out to be chemically homogeneous, with a metallicity Z ≈ 0.014 and a non-solar abundance mix. The availability of accurate and precise abundances eliminates one of the two variables in the opacity calculations for asteroseismic applications, allowing to focus on (missing) atomic data.

Keywords

stars: abundancesstars: atmospheresstars: early-typestars: variables: other
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 485 - 488
Copyright
Copyright © International Astronomical Union 2016 

References

Aerts, C., Christensen-Dalsgaard, J.,& Kurtz, D. W. 2010,Asteroseismology (Dordrecht: Springer)CrossRefGoogle Scholar
Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A 47 481 (AGSS09)Google Scholar
Bailey, J. E., Nagayama, T., Loisel, G. P., et al. 2015, Nature, 517, 56 CrossRefGoogle Scholar
Becker, S. R. 1998, ASP Conf. Ser., 131, 137 Google Scholar
Becker, S. R. & Butler, K. 1988, A&A, 201, 232 Google Scholar
Becker, S. R. & Butler, K. 1990, A&A, 235, 326 Google Scholar
Butler, K. & Giddings, J. R. 1985, Newsl. Analysis of Astron. Spectra, No. 9 (Univ. London)Google Scholar
Caffau, E., Ludwig, H.-G., Steffen, M., et al. 2011, Sol. Phys. 268 255 (CLSFB11)CrossRefGoogle Scholar
Ekström, S., Georgy, C., Eggenberger, P., et al. 2012, A&A, 537, A146 Google Scholar
Esteban, C., Peimbert, M., García-Rojas, J., et al. 2004, MNRAS, 355, 229 CrossRefGoogle Scholar
Giddings, J. R. 1981, Ph.D. Thesis (Univ. London)Google Scholar
Grevesse, N. & Sauval, A. J. 1998, Space Sci. Rev. 85 161 (GS98)CrossRefGoogle Scholar
Kurucz, R. L. 1993, CD-ROM No. 13 (Cambridge, Mass: SAO)Google Scholar
Maeder, A., Przybilla, N., Nieva, M. F., et al. 2014, A&A, 565, A39 Google Scholar
Morel, T., Butler, K., Aerts, C., Neiner, C., & Briquet, M. 2006, A&A, 457, 651 Google Scholar
Morel, T. & Butler, K. 2008, A&A, 487, 307 Google Scholar
Niemczura, E. & Daszyńska-Daszkiewicz, J. 2005, A&A, 433, 659 Google Scholar
Nieva, M. F. & Przybilla, N. 2006, ApJ (Letters), 639, L39 CrossRefGoogle Scholar
Nieva, M. F. & Przybilla, N. 2007, A&A, 467, 295 Google Scholar
Nieva, M. F. & Przybilla, N. 2008, A&A, 481, 199 Google Scholar
Nieva, M. F. & Przybilla, N. 2012, A&A 539 A143 (NP12)Google Scholar
Nieva, M. F. & Simón-Díaz, S. 2011, A&A 532 A2 (NSD11)Google Scholar
Przybilla, N. 2005, A&A, 443, 293 Google Scholar
Przybilla, N. & Butler, K. 2001, A&A, 379, 955 Google Scholar
Przybilla, N., Butler, K., Becker, S. R., et al. 2000, A&A, 359, 1085 Google Scholar
Przybilla, N., Butler, K., Becker, S. R., & Kudritzki, R. P. 2001, A&A, 369, 1009 Google Scholar
Przybilla, N., Nieva, M. F., & Butler, K. 2008, ApJ (Letters), 688, L103 CrossRefGoogle Scholar
Przybilla, N., Nieva, M. F., & Butler, K. 2011, J. Phys.: Conf. Ser., 328, 012015 Google Scholar
Salmon, S., Montalbán, J., Morel, T., et al. 2012, MNRAS, 422, 3460 CrossRefGoogle Scholar