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Asteroseismic Diagnostics for Semi-Convection in B Stars in the Era of K2

Published online by Cambridge University Press:  23 January 2015

Ehsan Moravveji
Ehsan Moravveji*
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium email: Ehsan.Moravveji@ster.kuleuven.be
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Abstract

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Semi-convection is a slow mixing process in chemically-inhomogeneous radiative interiors of stars. In massive OB stars, it is important during the main sequence. However, the efficiency of this mixing mechanism is not properly gauged yet. Here, we argue that asteroseismology of β Cep pulsators is capable of distinguishing between models of varying semi-convection efficiencies. We address this in the light of upcoming high-precision space photometry to be obtained with the Kepler two-wheel mission for massive stars along the ecliptic.

Keywords

asteroseismologystars: oscillations (including pulsations)stars: interiorsstars: evolutionstars: rotationvariables: others
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 182 - 187
Copyright
Copyright © International Astronomical Union 2015 

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