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Flare Magnetic Reconnection Dynamics Inferred from Flare Ribbons: Oscillations in the Reconnection Flux Rates and HXR Emission.

Presentation #106.12 in the session Solar Eruptive Events: Posters.

Published onSep 18, 2023
Flare Magnetic Reconnection Dynamics Inferred from Flare Ribbons: Oscillations in the Reconnection Flux Rates and HXR Emission.

Magnetic reconnection is understood to be the main physical process that transforms magnetic energy into heat, motion and particle acceleration in flares. Yet, observational constraints on magnetic and plasma properties of the reconnection region, and the dynamics that occur there are limited because of the high cadence and spatial resolution needed to capture these during a flare. Hard X-Ray (HXR) emission during flares allows us to indirectly understand properties of the magnetic reconnection process related to particle acceleration. To estimate the magnetic reconnection flux and its rate of change with time we study the evolution and morphology of post-reconnected field-line footpoints, or flare ribbons. Using 1600 Å Atmospheric Imaging Assembly (AIA) and the Helioseismic Magnetic Imager (HMI) vector photospheric magnetic fields we estimate the magnetic reconnection flux and rate, which allow us to probe dynamics of the current sheet above. We compare high resolution data from the Slit-Jaw Imager (SJI) onboard the Interface Region Imaging Spectrograph (IRIS) to study the evolution of fine-structures in the flare ribbon as they spread away from the polarity inversion line. We study the temporal relationship between the evolution of these fine structures and the quasi-periodic pulsations (QPP’s) signatures in the derived reconnection rates. Additionally, we use the RibbonDB database to perform statistical analysis of 73 C- to X-class flares and identify the relationship between the QPP’s in the reconnection rate and HXR emission properties using multiple spectral (Fourier and Wavelet) analyses. We find that the QPP periods range from one to ten minutes and are nearly cotemporal. We discuss how current sheet plasmoids could explain these observations, and how future studies could explore the diagnostic potential of these QPP observations.

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