Abstract
Self-consistent magnetohydrodynamic simulations of the solar corona with fine (\(\lesssim10\) km) grid scales are now being realized in parallel to advancements in high-resolution coronal spectropolarimetry provided by the National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST). We investigate the synthesis of polarized emission in the presence of apparent coronal fine structure exhibited by 3D MURaM coronal simulations for the key polarized spectral lines targeted by DKIST, namely Fe xiv\(\lambda5303\), Fe xi\(\lambda7892\), Fe xiii\(\lambda10746\), Fe xiii\(\lambda10798\), Si x\(\lambda14301\), and Si ix\(\lambda39343\). To benchmark our calculations, we provide detailed comparisons between the employed polarized line formation theory and established scalar line synthesis tools provided by the Chianti database team. To accelerate polarized synthesis for large simulations, we create efficient lookup tables based on atomic models significantly larger than previous studies. The spectral data cubes we describe provide a useful guide for the new era of multi-spectral DKIST coronal diagnostics as we discuss specific analysis techniques and challenges.
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Notes
At the time of writing, Chianti version 9 is the latest released version (https://www.chiantidatabase.org). Note that the Fe xiii atomic model used in CLE06 was negatively impacted by erroneous collisional data originally included in Chianti version 5 and later corrected in version 5.2.1.
Note that a bug in CLE06 caused most transitions other than E1, E2, and M1 to be ignored.
See https://cython.org/.
The code is open for use. Please contact the author for further information.
Atomic alignment refers to the imbalance of magnetic sublevel populations for different absolute values of magnetic quantum number. The angular distribution of radiative intensity for \(\pi\) and \(\sigma\) transitions between sublevels of two levels differ (see, e.g., Section 3.8 of Budker, Kimball, and DeMille, 2008)
Restricting the smallest example to 27 levels is somewhat arbitrarily selected for comparison; though, it does correspond to the number of levels originally included for the largest calculations of Fe xiii in CLE06.
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Acknowledgements
The National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation. The authors extend their thanks to Matthias Rempel, Phil Judge and Roberto Casini. Chianti is a collaborative project involving George Mason University, the University of Michigan (USA), University of Cambridge (UK) and NASA Goddard Space Flight Center (USA).
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Schad, T., Dima, G. Forward Synthesis of Polarized Emission in Target DKIST Coronal Lines Applied to 3D MURaM Coronal Simulations. Sol Phys 295, 98 (2020). https://doi.org/10.1007/s11207-020-01669-1
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DOI: https://doi.org/10.1007/s11207-020-01669-1