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Realistic 3D MHD Models of Flare-driven Quasi-Periodic Fast Magnetosonic Waves in Coronal Active Regions

Presentation #206.02 in the session Flare and CME Modeling and Observations.

Published onSep 18, 2023
Realistic 3D MHD Models of Flare-driven Quasi-Periodic Fast Magnetosonic Waves in Coronal Active Regions

Recent high resolution high cadence observations of coronal active regions (ARs) with SDO/AIA and with other spacecraft show ample evidence of MHD waves. The intermittent energy release often manifested as quasi-periodic pulsations in a flare likely produces the observed waves, where the location, directionality, and magnitude of the flare, as well as the AR magnetic geometry determine the wave properties. Propagating quasi-period fast magnetosonic (QFP) wave trains associated with flare pulsations were analyzed and studied using idealized 3D MHD models of bi-polar ARs. In the present study we extend the previous models by including realistic magnetic configuration based on force-free field (FFF) extrapolation with gravitationally stratified corona to initialize the model. The effects of the flare pulsations are modeled with a periodic driver that perturbs the magnetic footpoints in a localized region at the coronal base of the AR. We investigate various excitation parameters of the waves, as well as the effects of flare location, and compare to observations in the realistic AR magnetic geometry. We calculate the synthetic emission measure (EM) maps from the 3D MHD model output and compare to EUV observations. We investigate the dissipation of these waves in the coronal magnetic structures. We find that the 3D MHD model reproduces the main observed properties of the QFP waves, while improving the modeling of the emission details provides better understanding of the QFP wave generation and propagation properties. These realistic 3D simulations are a necessary step towards practical applications of coronal seismology as well as for evaluating the contribution of these waves to coronal heating.

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