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Systematic Study of L-Shell Opacity at Stellar Interior Temperatures.

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This study measured chromium and nickel opacity at stellar interior temperatures, finding smaller model discrepancies than for iron. Discrepancies suggest opacity models need refinement for density effects and excited states.

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Area of Science:

  • Plasma physics
  • Astrophysical opacity
  • Atomic physics

Background:

  • Accurate opacity measurements are crucial for stellar modeling.
  • Previous experiments showed discrepancies between measured and modeled iron opacity at stellar interior temperatures.
  • Systematic studies are needed to understand opacity dependence on atomic number.

Purpose of the Study:

  • To systematically study opacity dependence on atomic number at stellar interior temperatures.
  • To evaluate discrepancies between measured and modeled iron, chromium, and nickel opacity.
  • To identify shortcomings in current opacity models.

Main Methods:

  • Measured high-temperature (>180 eV) chromium and nickel opacities using methods similar to previous iron opacity experiments.
  • Ensured experiment reliability through 10%-20% reproducibility.
  • Compared experimental data with theoretical opacity models.

Main Results:

  • High-temperature chromium and nickel opacities were measured with 6%-10% uncertainty.
  • Overall model-data disagreements were smaller for chromium and nickel than for iron.
  • Shortcomings in models were identified for density effects, excited states, and open L-shell configurations.
  • A significant underestimate (30%-45%) in modeled quasicontinuum opacity at short wavelengths was observed for iron, but not for chromium or nickel, at temperatures above 180 eV.

Conclusions:

  • Opacity models exhibit shortcomings in accurately predicting opacity for elements with open L-shell configurations and at high densities.
  • The unique discrepancy observed for iron opacity suggests either missing physics in opacity theories or an experimental artifact specific to iron at high temperatures.
  • Further research is needed to resolve the iron opacity discrepancy and improve theoretical models for astrophysical applications.