Opacity calculations for stellar astrophysics. (arXiv:1901.08959v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Pain_J/0/1/0/all/0/1">Jean-Christophe Pain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilleron_F/0/1/0/all/0/1">Franck Gilleron</a>
Opacity is a key ingredient of stellar structure and evolution. In the
present work, we recall the role of opacity in asteroseismology, focusing
mainly on two kinds of astrophysical objects: $beta$ Cephei-type stars, and
the Sun. The detailed opacity code SCO-RCG for local-thermodynamic-equilibrium
plasmas is described and interpretation of laser and Z-pinch experiments are
presented and discussed. The possible role of multi-photon processes on
radiative accelerations is outlined, and the main aspects of opacity modeling
which should be improved are mentioned.
Opacity is a key ingredient of stellar structure and evolution. In the
present work, we recall the role of opacity in asteroseismology, focusing
mainly on two kinds of astrophysical objects: $beta$ Cephei-type stars, and
the Sun. The detailed opacity code SCO-RCG for local-thermodynamic-equilibrium
plasmas is described and interpretation of laser and Z-pinch experiments are
presented and discussed. The possible role of multi-photon processes on
radiative accelerations is outlined, and the main aspects of opacity modeling
which should be improved are mentioned.
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