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EP: Fachverband Extraterrestrische Physik

EP 6: Sun and Heliosphere I

EP 6.1: Hauptvortrag

Mittwoch, 18. März 2026, 13:45–14:15, KH 01.019

Simulation of the photosphere and chromospheres of sunspots — •Aswathi Krishnan Kutty, Robert H. Cameron, Damien Przybylski, Tanayveer Bhatia, and Sami K. Solanki — Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Goettingen

Sunspots are one of the most prominent features of the solar surface and are characterized by a dark central core called the umbra, which is surrounded by a collection of filamentary structures called the penumbra. The penumbra is on average considerably brighter than the umbra but darker than the surrounding quiet Sun. At the photospheric level, the nearly horizontal Evershed flow is directed outward from the outer edge of the umbra along penumbral filaments. On the other hand, in the chromosphere, the flow is reversed and the plasma flows inwards towards the umbra. Radiative magneto-hydrodynamic (rMHD) codes have simulated sunspots in the upper convection zone and photosphere (Heinemann et al., 2007; Rempel et al., 2009). However, simulations of sunspots that include a realistic treatment of the chromosphere and corona have not yet been performed. The structure and evolution of the chromospheric field will be important in understanding magnetic reconnection and processes that are important for flare initiation. In this talk, I will present the first simulations of sunspots that reach layers above the solar photosphere.

Keywords: sunspots; MURaM; Radiative Magnetohydrodynamics; chromosphere