Three-dimensional Magnetohydrodynamic Shocks and Associated Plasma Heating in the Solar Atmosphere
Abstract
We investigate the three-dimensional (3D) formation and evolution of magnetohydrodynamic (MHD) shock waves and their role in plasma heating within a solar bipolar active region. Using 3D compressible, resistive MHD simulations, we model the emergence of magnetic flux from the convection zone into a magnetized corona. Our results reveal that initial plasmoid ejections launch hot plasma jets preceded by slow-mode shocks. Unlike established 2D models, these ejections originate from multiple sites along the emerging field's periphery, resulting in shocks with a complex, inverted-U 3D morphology. Beneath these fronts, the heated plasma forms flattened, sheet-like columns. Furthermore, we find that sustained gas pressure gradients, driven by dense plasma accumulation from plasmoids, power a cool, dense upflow adjacent to the main reconnection jet. During the main reconnection phase, the collision of ejected plasmoids with the ambient field triggers the formation of fast-mode termination shocks. By mapping viscous heating directly onto these irregular 3D shock surfaces, we demonstrate that energy dissipation is highly localized. This finding provides a physical link between shock-induced viscous heating and the observed temperature enhancements at the apex of post-flare loops.
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BibTeX
@misc{giannis2026threedimensional,
title = {{Three-dimensional Magnetohydrodynamic Shocks and Associated Plasma Heating in the Solar Atmosphere}},
author = {Angelos Giannis and Vasilis Archontis},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.36932},
eprint = {2610.36932},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.36932},
}
RIS
TY - UNPB
TI - Three-dimensional Magnetohydrodynamic Shocks and Associated Plasma Heating in the Solar Atmosphere
AU - Angelos Giannis
AU - Vasilis Archontis
PY - 2026
DA - 2026/10/27
PB - arXiv
DO - 10.48550/arxiv.2610.36932
UR - https://arxiv.org/abs/2610.36932
AB - We investigate the three-dimensional (3D) formation and evolution of magnetohydrodynamic (MHD) shock waves and their role in plasma heating within a solar bipolar active region. Using 3D compressible, resistive MHD simulations, we model the emergence of magnetic flux from the convection zone into a magnetized corona. Our results reveal that initial plasmoid ejections launch hot plasma jets preceded by slow-mode shocks. Unlike established 2D models, these ejections originate from multiple sites along the emerging field's periphery, resulting in shocks with a complex, inverted-U 3D morphology. Beneath these fronts, the heated plasma forms flattened, sheet-like columns. Furthermore, we find that sustained gas pressure gradients, driven by dense plasma accumulation from plasmoids, power a cool, dense upflow adjacent to the main reconnection jet. During the main reconnection phase, the collision of ejected plasmoids with the ambient field triggers the formation of fast-mode termination shocks. By mapping viscous heating directly onto these irregular 3D shock surfaces, we demonstrate that energy dissipation is highly localized. This finding provides a physical link between shock-induced viscous heating and the observed temperature enhancements at the apex of post-flare loops.
ER -