Coronal oscillations in the self-consistent 3D MHD simulations of the solar atmosphere
Abstract
Solar coronal loops are commonly subject to oscillations. Coronal oscillations are typically studied using highly idealised models of magnetic flux-tubes. In order to improve our understanding of coronal oscillations, it is necessary to consider the effect of realistic magnetic field topology and evolution. To do this, we study excitation, evolution and damping of coronal oscillations in three-dimensional self-consistent simulations of solar atmosphere spanning from convection zone to solar corona using the radiation-MHD code Bifrost. We use forward-modelled EUV emission and three-dimensional tracing of magnetic field to analyse oscillatory behaviour of individual magnetic loops. We show that coronal loop oscillations are abundant in such models and the oscillation modes and characteristics match those detected in solar observations. Finally, we discuss the dynamics and variability of the oscillating loops and the implications for coronal seismology.
- Publication:
-
44th COSPAR Scientific Assembly. Held 16-24 July
- Pub Date:
- July 2022
- Bibcode:
- 2022cosp...44.2494K