Abstract
We present opacity calculations with the newly developed STAR code, which implements the Super-Transition-Array (STA), with various improvements. The model is used to calculate and analyze local thermodynamic equilibrium opacities of mid and high Z elements and of the solar interior plasma. We briefly review the underlying computational model and present calculations for iron and neodymium over a wide range of temperature and density.
Highlights
The calculation of atomic opacities from first principles is an important part in the modeling of various astrophysical phenomena, and especially the physics of stellar interior
Opacities quantify the strong coupling between radiation and matter in a hot dense plasma, and are directly related to the radiative thermal conductivity in stellar interior
Metallic elements have a significant contribution to the opacity in the solar interior, they only constitute a few percent of the mixture, since these metallic elements are not completely ionized and give rise to strong bound-bound and bound-free absorption
Summary
The calculation of atomic opacities from first principles is an important part in the modeling of various astrophysical phenomena, and especially the physics of stellar interior. Metallic elements have a significant contribution to the opacity in the solar interior, they only constitute a few percent of the mixture, since these metallic elements are not completely ionized and give rise to strong bound-bound and bound-free absorption. This gives rise to a connection between the solar composition problem and the theoretical uncertainty in the calculation of opacities at stellar interior conditions [4,5,6,7]. We present maps for the contributions of the different atomic processes to the Rosseland opacity
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