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

被引：37
作者：
Walczak, Przemyslaw [1 ]
Fontes, Christopher J. [2 ]
Colgan, James [3 ]
Kilcrease, David P. [3 ]
Guzik, Joyce A. [4 ]
机构：
[1] Uniwersytet Wroclawski, Inst Astron, PL-51622 Wroclaw, Poland
[2] Los Alamos Natl Lab, Computat Phys Div, Los Alamos, NM 87545 USA
[3] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA
[4] Los Alamos Natl Lab, Theoret Design Div, Los Alamos, NM 87545 USA
来源：
ASTRONOMY & ASTROPHYSICS | 2015年 / 580卷
关键词：
asteroseismology; atomic data; opacity; stars: oscillations; LIGHT-ELEMENT OPACITIES; MODE-IDENTIFICATION; EXCITATION; STELLAR; MODULES;
D O I：
10.1051/0004-6361/201526824
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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 beta 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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页数：4
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