Speaker
Description
First Name: Damien
Last Name: Przybylski
Email Address: przybylski@mps.mpg.de
Affiliation: Max Planck Institute for Solar System Research
All Authors: D. Przybylski
Abstract: The solar chromosphere presents a formidable modelling challenge. The coupling of the turbulent convection zone to the underlying magnetic field leads to it's highly dynamic nature, displaying spicules, shocks, swirls and jets. The large-scale magnetic topology further impacts the observed chromosphere. Finally a non-local thermodynamic equilibrium (NLTE) treatment is required. Capturing this multi-scale, multi-physics regime has long exceeded computational capabilities. With increasing computational power, 3D models are now able to include approximations to NLTE physics and non-equilibrium ionization. At the same time, larger simulations including more realistic magnetic topologies can be performed. Finally, spectral lines can be synthesised with 3D radiative transfer allowing for more accurate comparison between simulation and observation. In this contribution, we review current chromospheric modelling, outlining the capabilities and limitations. Models are now able to match the average line widths and intensities, yet discrepencies remain. We propose that a spatially resolved multi-height approach is now required to understand these differences, including the local magnetic field strength and flux imbalance, chromospheric lines and optically thin coronal observables.