Solar granulation-generated chromospheric heating and plasma outflows in two-fluid magnetic arcade
- 1Institute of Physics, Maria Curie-Skłodowska University, Lublin, Poland (mayankgis786@gmail.com)
- 2Particle Physics and Universe Sciences (PAPU), Department of Physics, University of Helsinki, Helsinki, Finland (mayankgis786@gmail.com)
- 3Shenzhen Key Laboratory of Numerical Prediction for Space Storm, Institute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, People’s Republic of China, 51805 (kuzma@hit.edu.cn)
- 4Centre for Mathematical Plasma Astrophysics, KU Leuven, 3001 Leuven, Belgium
- 5Solar Physics & Space Plasma Research Centre, School of Mathematics and Statis- tics, University of Sheffield, United Kingdom
Context. The heating of the solar chromosphere, the associated plasma outflows, and the origin of the solar wind are key issues in heliophysics. In this paper, we provide a new perspective on their connection to the propagation and dissipation of waves generated by solar granulation.
Aims. The primary objective of this paper is to conduct 2.5-D numerical simulations of the partially ionized lower solar atmosphere, investigating the propagation and dissipation of granulation-generated waves in the context of plasma outflows and the related heating of the chromosphere, which is due to ion-neutral collisions.
Methods. We use the JOint ANalytical and Numerical Approach (JOANNA) code to solve the two-fluid model equations. We take into account partially ionized hydrogen plasma composed of ions (protons) and neutrals (H atoms), which are coupled via ion-neutral collisions. We focus on a quiet region of the solar chromosphere which is gravitationally stratified and magnetically constrained by an initially set magnetic Plasma flows and solar chromosphere heating arcade. Solar convection situated beneath the photosphere is the main source of these waves that are propagating through the simulated solar atmosphere.
Results. The numerical results obtained in our study reveal an important process in the lower solar atmosphere. The naturally evolving convection generates waves and a portion of the wave energy is dissipated due to ion-neutral collisions in the solar chromosphere. This dissipation of waves, in turn, leads to the release of thermal energy, resulting in the heating of the solar atmosphere. This phenomenon is also associated with upward-directed plasma flows, which may play a role in the formation of the solar wind. Furthermore, our analysis of the dominant wave periods in the various layers
of the solar atmosphere closely aligns with observational data from Wiśniewska et al. (2016) and Kayshap et al. (2018). This alignment underscores the crucial role ion-neutral collisions play in facilitating the energy release process, shedding light on the intricate dynamics of the solar atmosphere.
Conclusions. Based on our numerical simulations, we can draw the following conclusions: The dissipation of waves in the two-fluid plasma caused by ion-neutral collisions in the two-fluid plasma model leads to plasma outflows and increased heating in the chromosphere. These plasma outflows may play a role in the generation of the solar wind and the accompanying heating.
How to cite: Kumar, M., Murawski, K., Kuźma, B., Kadowaki, L., Kilpua, E., Poedts, S., and Erdelyi, R.: Solar granulation-generated chromospheric heating and plasma outflows in two-fluid magnetic arcade, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-2303, https://doi.org/10.5194/egusphere-egu24-2303, 2024.
