Speaker
Description
Understanding the formation and dynamics of cool solar loops is essential for unraveling the complex energy transport mechanisms in the solar atmosphere. In this talk, we will focus on the formation of cool loops driven by Alfvén pulses under ideal and non-ideal magnetohydrodynamic (MHD) regimes. Using 2.5D MHD simulations in a gravitationally stratified model solar atmosphere, we demonstrate how multiple transverse pulses that resemble Alfvén pulses, may nonlinearly transfer energy and momentum to field-aligned perturbations via the ponderomotive force. This interaction leads to the generation of magnetoacoustic shocks and the subsequent plasma motions that is responsible for the formation of cool plasma loops along curved magnetic field lines. In the ideal MHD case, the resulting plasma flows exhibit a periodicity of approximately 4 minutes, while the trailing wave signatures show a 2-minute periodicity. We further explore the influence of non-ideal effects, including thermal conduction and radiative cooling, on the thermal structure and evolution of these loops. Our results suggest that impulsive Alfvén pulses may play a significant role in the formation of short, cool loops in the solar atmosphere. These findings offer new insights into wave-driven loop dynamics and have implications for interpreting high-resolution observations from missions such as IRIS. They also contribute to our understanding of localized coronal heating and wave dissipation mechanisms in structured solar atmosphere.
| Sessions | Wave generation, energy transport, dissipation and heating |
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