Reduced atomic models for large-scale computations: Fe XIII near-infrared lines
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arXiv
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| Autores principales: | , |
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| Formato: | Preprint |
| Publicado: |
2025
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| _version_ | 1866910871949672448 |
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| author | Del Zanna, Giulio Dayananda, Supriya Hebbur |
| author_facet | Del Zanna, Giulio Dayananda, Supriya Hebbur |
| contents | Accurate atomic models for astrophysical plasma can be very complex, requiring thousands of states. However, for a variety of applications such as large-scale forward models of the Stokes parameters of a spectral line in the solar corona, it is necessary to build much reduced atomic models. We present two examples of such models, focused on the two near-infrared Fe XIII lines observed on the ground at 10750, 10801 Angstroms. These lines are primary diagnostics for a range of missions (especially the Daniel K. Inouye Solar Telescope, DKIST) to measure electron densities and magnetic fields in the solar corona. We calculate the Stokes parameters for a range of coronal conditions using CHIANTI (for intensities) and P-CORONA (for intensities and polarization), and use P-CORONA and a realistic global MHD simulation to show that the reduced models provide accurate results, typically to within 5% those obtained with larger models. Reduced models provide a significant decrease (over three orders of magnitude) in the computational time in spectropolarimetric calculations. The methods we describe are general and can be applied to a range of conditions and other ions. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_09540 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Reduced atomic models for large-scale computations: Fe XIII near-infrared lines Del Zanna, Giulio Dayananda, Supriya Hebbur Solar and Stellar Astrophysics Atomic Physics Accurate atomic models for astrophysical plasma can be very complex, requiring thousands of states. However, for a variety of applications such as large-scale forward models of the Stokes parameters of a spectral line in the solar corona, it is necessary to build much reduced atomic models. We present two examples of such models, focused on the two near-infrared Fe XIII lines observed on the ground at 10750, 10801 Angstroms. These lines are primary diagnostics for a range of missions (especially the Daniel K. Inouye Solar Telescope, DKIST) to measure electron densities and magnetic fields in the solar corona. We calculate the Stokes parameters for a range of coronal conditions using CHIANTI (for intensities) and P-CORONA (for intensities and polarization), and use P-CORONA and a realistic global MHD simulation to show that the reduced models provide accurate results, typically to within 5% those obtained with larger models. Reduced models provide a significant decrease (over three orders of magnitude) in the computational time in spectropolarimetric calculations. The methods we describe are general and can be applied to a range of conditions and other ions. |
| title | Reduced atomic models for large-scale computations: Fe XIII near-infrared lines |
| topic | Solar and Stellar Astrophysics Atomic Physics |
| url | https://arxiv.org/abs/2503.09540 |