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The Wootton center for astrophysical plasma properties: First results for helium

Published online by Cambridge University Press:  12 October 2020

M. H. Montgomery Open the ORCID record for M. H. Montgomery [Opens in a new window] ,
D. E. Winget ,
M.-A. Schaeuble ,
B. H. Dunlap  and
J. T. Fuchs
M. H. Montgomery
Affiliation:
Department of Astronomy and McDonald Observatory University of Texas, Austin, Texas78712, USA emails: [email protected], [email protected], [email protected]
D. E. Winget
Affiliation:
Department of Astronomy and McDonald Observatory University of Texas, Austin, Texas78712, USA emails: [email protected], [email protected], [email protected]
M.-A. Schaeuble
Affiliation:
Sandia National Laboratories, Albuquerque, New Mexico87123, USA email: [email protected]
B. H. Dunlap
Affiliation:
Department of Astronomy and McDonald Observatory University of Texas, Austin, Texas78712, USA emails: [email protected], [email protected], [email protected]
J. T. Fuchs
Affiliation:
Department of Physics, Texas Lutheran University, Seguin, Texas78155, USA email: [email protected]
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Abstract

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The Wootton Center for Astrophysical Plasma Properties (WCAPP) is a new center focusing on the spectroscopic properties of stars and accretion disks using “at-parameter” experiments. Currently, these experiments use the X-ray output of the Z machine at Sandia National Laboratories — the largest X-ray source in the world — to heat plasmas to the same conditions (temperature, density, and radiation environment) as those observed in astronomical objects. The experiments include measuring (1) density-dependent opacities of iron-peak elements at solar interior conditions, (2) spectral lines of low-Z elements at white dwarf photospheric conditions, (3) atomic population kinetics of neon in a radiation-dominated environment, and (4) resonant Auger destruction (RAD) of silicon at conditions found in accretion disks around supermassive black holes. In particular, we report on recent results of our experiments involving helium at white dwarf photospheric conditions. We present results showing disagreement between inferred electron densities using the Hβ line and the He I 5876 Å line, most likely indicating incompleteness in our modeling of this helium line.

Keywords

atomic dataatomic processesmethods: laboratory
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 231 - 236
Copyright
© International Astronomical Union 2020

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