Abstract Details


Name: Anoop K Mathew
Affiliation: National Institute of Technology Calicut
Conference ID: TVS202510296
Title: Temporal and Spatial Evolution of Flare Ribbons During the X1.1-Class Solar Flare of 23 March 2024.
Authors and Co-Authors: Ram Ajor Maurya
Abstract Type: Contributory Presentation
Abstract: A comprehensive multi-wavelength investigation was conducted on the X1.1-class solar flare that erupted on 23 March 2024 from NOAA Active Region 13614, focusing on the evolution of flare ribbons and underlying magnetic reconnection processes. Utilizing coordinated data from SDO/AIA ultraviolet and extreme ultraviolet channels, SDO/HMI magnetograms, and GOES soft X-ray sensors, the study traced the temporal and spatial dynamics of the event. The flare was characterized by the progressive separation of two bright flare ribbons across the polarity inversion line (PIL), correlated with strong energy release, plasma heating, and restructuring of magnetic fields. Peak ribbon separation velocities exceeded 130 kms−1 during the flare’s impulsive phase, while average values remained consistent with those observed in large eruptive flares. These findings reinforce the standard magnetic reconnection framework for solar flare energetics and morphology. The total magnetic free energy and its temporal evolution are estimated through rigorous comparison of pre-flare and post-flare magnetic field models. By correlating flare ribbon separation speeds derived from ultraviolet imaging with theoretical reconnection rates predicted by the standard flare model, we quantitatively assess the partitioning of released magnetic energy into plasma heating, particle acceleration, and bulk motions. Our results reveal a close correspondence between peak energy release epochs and the most impulsive phases of ribbon separation, indicating efficient energy transfer from magnetic restructuring to observable chromospheric and coronal signatures.