3D RT in a MURaM-ChE enhanced network simulation produces Mg II h&k lines closer to IRIS data than 1.5D, showing larger 1.5D-3D discrepancies than Bifrost due to horizontal velocities and more scatter in correlations.
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Simulations identify photospheric magnetic field strength as the main driver of Mg II core line widths in quiet Sun regions, with non-equilibrium hydrogen ionization and 3D radiative transfer key in active regions.
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Mg II h&k spectral line properties computed using 3D radiative transfer in an enhanced network region simulated with the MURaM-ChE code
3D RT in a MURaM-ChE enhanced network simulation produces Mg II h&k lines closer to IRIS data than 1.5D, showing larger 1.5D-3D discrepancies than Bifrost due to horizontal velocities and more scatter in correlations.
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Chromospheric dynamics and the O I 135.6~nm spectral line
Simulations identify photospheric magnetic field strength as the main driver of Mg II core line widths in quiet Sun regions, with non-equilibrium hydrogen ionization and 3D radiative transfer key in active regions.