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EP: Fachverband Extraterrestrische Physik
EP 10: Poster Session
EP 10.18: Poster
Donnerstag, 3. April 2025, 11:00–12:30, ZHG Foyer 1. OG
Diagnostics of comprehensive simulations of the chromosphere — •Patrick Alexander Ondratschek1, Damien Przybylski1, H.N. Smitha1, Robert Cameron1, Sami K. Solanki1, and Jorrit Leenaarts2 — 1Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany — 2Institute for Solar Physics, Stockholm, Sweden
The chromosphere is a region of the solar atmosphere above the photosphere and below the millions of Kelvin hot corona. It is a place of extremes where multiple physical transitions take place. In the photosphere, the dynamics are dominated by the plasma pressure. As the density decreases with height, the magnetic field becomes dynamically important. The detailed processes that heat the chromosphere and provide the mass for the corona are only poorly understood. Many studies of the chromosphere are based on a few strong spectral lines that carry the necessary diagnostic potential to infer physical quantities such as e.g. temperature, velocity, and magnetic field. These spectral lines form under nonlocal thermodynamic equilibrium conditions and are difficult to interpret. We aim to understand line formation in the solar chromosphere by synthesizing spectral lines from numerical models. Previous models of the solar chromosphere resulted in too-faint intensities and too-narrow line widths when compared with observations. We use a new model of the chromosphere simulated with the MURaM-ChE code to study the formation of the Mg II h&k and Ca II 8542 lines. We find an improved match with the observations, signifying a step forward in our understanding of the chromosphere.
Keywords: Chromosphere; Radiative transfer; Forward modeling