A new generation of Los Alamos opacity tables

Colgan, J.; Kilcrease, D. P.; Magee, N. H.; Abdallah, J.; Sherrill, M. E.; Fontes, C. J.; Hakel, P.; Guzik, Joyce A.; Mussack, Katie; Walczak, P.

doi:10.1063/1.4975741

Cited by 4 publications

(6 citation statements)

References 67 publications

(73 reference statements)

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“…The vertical dotted line marks the temperature at the base of the convection zone in the present Sun. Courtesy of H. M. Antia calculations, in the OPLIB tables (Colgan et al 2016). A review of these recent opacity results was provided by Turck-Chièze et al (2016), while Fig.…”

Section: Opacitymentioning

confidence: 99%

Solar structure and evolution

Christensen‐Dalsgaard

2021

Living Rev Sol Phys

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The Sun provides a critical benchmark for the general study of stellar structure and evolution. Also, knowledge about the internal properties of the Sun is important for the understanding of solar atmospheric phenomena, including the solar magnetic cycle. Here I provide a brief overview of the theory of stellar structure and evolution, including the physical processes and parameters that are involved. This is followed by a discussion of solar evolution, extending from the birth to the latest stages. As a background for the interpretation of observations related to the solar interior I provide a rather extensive analysis of the sensitivity of solar models to the assumptions underlying their calculation. I then discuss the detailed information about the solar interior that has become available through helioseismic investigations and the detection of solar neutrinos, with further constraints provided by the observed abundances of the lightest elements. Revisions in the determination of the solar surface abundances have led to increased discrepancies, discussed in some detail, between the observational inferences and solar models. I finally briefly address the relation of the Sun to other similar stars and the prospects for asteroseismic investigations of stellar structure and evolution.

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Section: Opacitymentioning

confidence: 99%

Solar structure and evolution

Christensen‐Dalsgaard

2021

Living Rev Sol Phys

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“…The ATOMIC-code [39,40] "full" calculations allow single-configuration fine-structure detail to be included in a relatively computationally inexpensive manner. They thus include intermediate coupling within a configuration but not complete interaction among the set of configurations.…”

Section: Comparisons Of Rosseland Meansmentioning

confidence: 99%

“…Figure 7. Comparison between SCO-RCG and ATOMIC "full" (left) and "n5" (right) computations [39][40][41] of iron opacity at T = 23 eV and ρ = 2 mg/cm 3 . The ATOMIC calculations were kindly provided by J. Colgan.…”

Section: Comparisons Of Rosseland Meansmentioning

confidence: 99%

“…The Rosseland means are rather close, although some differences exist around hν = 800 eV (maximum of the derivative of Planck's distribution with respect to temperature). [39,40] at the same conditions (right). The ATOMIC calculations were kindly provided by J. Colgan.…”

Section: The Boundary Of the Radiative/convective Zones Of The Sunmentioning

confidence: 99%

“…OP [42,43] 0.59 R-matrix [75,76] 0.51 ATOMIC [39,40] 0.60 OPAS [82][83][84] 0.70 SCO-RCG [17] 0.64 SCRAM [85] 0.77 TOPAZ [86,87] 0.62 Cold [72] 0.75…”

Section: Source κ R Relative To Experimentsmentioning

confidence: 99%

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Detailed Opacity Calculations for Astrophysical Applications

Pain

Gilleron

Comet

2017

Atoms

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Nowadays, several opacity codes are able to provide data for stellar structure models, but the computed opacities may show significant differences. In this work, we present state-of-the-art precise spectral opacity calculations, illustrated by stellar applications. The essential role of laboratory experiments to check the quality of the computed data is underlined. We review some X-ray and XUV laser and Z-pinch photo-absorption measurements as well as X-ray emission spectroscopy experiments involving hot dense plasmas produced by ultra-high-intensity laser irradiation. The measured spectra are systematically compared with the fine-structure opacity code SCO-RCG. The focus is on iron, due to its crucial role in understanding asteroseismic observations of β Cephei-type and Slowly Pulsating B stars, as well as of the Sun. For instance, in β Cephei-type stars, the iron-group opacity peak excites acoustic modes through the "kappa-mechanism". Particular attention is paid to the higher-than-predicted iron opacity measured at the Sandia Z-machine at solar interior conditions. We discuss some theoretical aspects such as density effects, photo-ionization, autoionization or the "filling-the-gap" effect of highly excited states.

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New Los Alamos Opacity Calculations

Colgan

Kilcrease

Magee

et al. 2018

Atoms

Self Cite

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In 2015 Los Alamos National Laboratory (LANL) released a new set of OPLIB opacity tables for the elements hydrogen through zinc. The new LANL opacities are publicly available via our website and are already in use by the astrophysics community. In this contribution, we discuss the extension of our opacity calculations to elements beyond zinc. Such calculations are motivated by potential industrial applications (for elements such as Sn) as well as available experimental data with which to compare our calculations (for Ge and Br). After a short outline of our method for computing opacities for these elements, we make comparisons to available experimental data and find good agreement. Future plans are briefly discussed.

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A new generation of Los Alamos opacity tables

Cited by 4 publications

References 67 publications

Solar structure and evolution

Solar structure and evolution

Detailed Opacity Calculations for Astrophysical Applications

New Los Alamos Opacity Calculations

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