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.

引用

页数：4