Wider pulsation instability regions for β Cephei and SPB stars calculated using new Los Alamos opacities

Aims. Our goal is to test the newly developed OPLIB opacity tables from Los Alamos National Laboratory and check their influence on the pulsation properties of B-type stars. Methods. We calculated models using MESA and Dziembowski codes for stellar evolution and linear, nonadiabatic pulsations, resp...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2015-08, Vol.580, p.L9
Main Authors: Walczak, Przemysław, Fontes, Christopher J., Colgan, James, Kilcrease, David P., Guzik, Joyce A.
Format: Article
Language:English
Subjects:
asteroseismology
ASTRONOMY AND ASTROPHYSICS
ATOMIC
ATOMIC AND MOLECULAR PHYSICS
atomic data
OP
opacity
OPAL
OPLIB
SPB
SPBsg
stars: oscillations
stars:variables:general
βCephei
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Summary:Aims. Our goal is to test the newly developed OPLIB opacity tables from Los Alamos National Laboratory and check their influence on the pulsation properties of B-type stars. Methods. We calculated models using MESA and Dziembowski codes for stellar evolution and linear, nonadiabatic pulsations, respectively. We derived the instability domains of β Cephei and SPB-types for different opacity tables OPLIB, OP, and OPAL. Results. The new OPLIB opacities have the highest Rosseland mean opacity coefficient near the so-called Z-bump. Therefore, the OPLIB instability domains are wider than in the case of OP and OPAL data.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361/201526824