Wider pulsation instability regions for β Cephei and SPB stars calculated using new Los Alamos opacities
Astronomy & Astrophysics, 2015•aanda.org
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 …
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 …
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.
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