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Iron-group opacities in the envelopes of massive stars

Published online by Cambridge University Press:  18 February 2014

Maëlle Le Pennec  and
Sylvaine Turck-Chièze
Maëlle Le Pennec
Affiliation:
CEA/DSM/IRFU/SAp, CE Saclay, 91191 Gif-sur-Yvette, France email: [email protected]; [email protected]
Sylvaine Turck-Chièze
Affiliation:
CEA/DSM/IRFU/SAp, CE Saclay, 91191 Gif-sur-Yvette, France email: [email protected]; [email protected]
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Abstract

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β Cephei and SPB stars are pulsating stars for which the excitation of modes by the κ mechanism, due to the iron-group opacity peak, seems puzzling. We have first investigated the origins of the differences noticed between OP and OPAL iron and nickel opacity calculations (up to a factor 2), a fact which complicates the interpretation. To accomplish this task, new well-qualified calculations (SCO-RCG, HULLAC and ATOMIC) have been performed and compared to values of these tables, and most of the differences are now well understood. Next, we have exploited a dedicated experiment on chromium, iron and nickel, conducted at the LULI 2000 facilities. We found that, in the case of iron, detailed calculations (OP, ATOMIC and HULLAC) show good agreement, contrary to all of the non-detailed calculations. However, in the case of nickel, OP calculations show large discrepancies with the experiments but also with other codes. Thus, the opacity tables need to be revised in the thermodynamical conditions corresponding to the peak of the iron group. Consequently we study the evolution of this iron peak with changes in stellar mass, age, and metallicity to determine the relevant region where these tables should be revised.

Keywords

opacityatomic dataatomic processesstars: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 229 - 232
Copyright
Copyright © International Astronomical Union 2014 

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