Göttingen 2025 – wissenschaftliches Programm

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EP: Fachverband Extraterrestrische Physik

EP 6: Sun and Heliosphere III

EP 6.6: Vortrag

Dienstag, 1. April 2025, 17:45–18:00, ZHG101

Comprehensive simulations of solar prominences — •Lisa-Marie Zessner, Robert Cameron, Sami K. Solanki, and Damien Przybylski — Max Planck Institute for Solar System Research, Göttingen, Germany

Solar prominences are cool and dense plasma clouds suspended in the hot solar corona. The heavy prominence plasma is supported against gravity by the magnetic field. Solar prominences are common features in the solar atmosphere, with diverse properties: they can have very different sizes, lifetimes, dynamics, and fine structures. If they become unstable, they can erupt and form the core of coronal mass ejections. Many aspects of their physics are still unknown, including their formation mechanism. We use the radiative magnetohydrodynamic code MURaM to simulate the formation and dynamics of a prominence in the solar atmosphere. MURaM includes the relevant physical processes to simulate the solar photosphere, chromosphere, and corona.

We create a stable, dipped magnetic arcade configuration in a 3D simulation box and let it evolve. In the course of the simulation, a solar prominence forms self-consistently. First, a dense plasma seed ejected from the chromosphere randomly settles into a magnetic dip of the field configuration and gets cooled by radiative losses. The resulting pressure drop then drives a strong inflow of hot plasma that condenses onto the feature. In this way, a dynamic, cool, and dense structure is built up in the solar corona. In this contribution, I will present the formation mechanism and properties of the simulated prominence for different setups of our configuration.

Keywords: Solar prominences; MHD simulations; MURaM