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Main-sequence oscillators as a test of stellar opacities

Published online by Cambridge University Press:  27 October 2016

Warrick H. Ball
Warrick H. Ball*
Affiliation:
Institut für Astrophysik, Georg-August-Universität Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany email: [email protected] Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
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Abstract

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The last decade has given rise to several tensions between calculated and (sometimes indirectly) measured stellar opacities. I discuss the current and future capacity for the asteroseismology of B-type oscillators (slowly-pulsating B-type stars and β Cepheids) and main-sequence solar-like oscillators to test stellar opacities. I briefly highlight two methods by which the B-type oscillators already constrain opacities, though they do not yet identify a superior set of tables. I then consider how the main-sequence solar-like oscillators might also test opacities, using the 16 Cygni system as an example. There are currently greater uncertainties than the opacities (in this example, the atmospheric structure) but many of these will be separately constrained in the near future.

Keywords

radiative transferstars: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 653 - 660
Copyright
Copyright © International Astronomical Union 2016 

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