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This work analyzes the Hall magnetohydrodynamics (HMHD) andmagnetohydrodynamics (MHD) numerical simulations of a flaring solar activeregion as a testbed while idealizing the coronal Alfv\'en speed to be of twoorders of magnitude lesser. HMHD supports faster magnetic reconnection andshows richer complexity in magnetic field line evolution compared to the MHD.The magnetic reconnections triggering the flare are explored by numericalsimulations augmented with relevant multi-wavelength observations. The initialcoronal magnetic field is constructed by non-force-free extrapolation ofphotospheric vector magnetic field. Magnetic structure involved in the flare isidentified to be a flux rope, with its overlying magnetic field linesconstituting the quasi-separatrix layers (QSLs) along with a three-dimensionalnull point and a null line. Compared to the MHD simulation, the HMHD simulationshows a higher and faster ascend of the rope together with the overlying fieldlines, which further reconnect at the QSL located higher up in the corona. Thefoot points of the field lines match better with the observations for the HMHDcase with the central part of the flare ribbon located at the chromosphere.Additionally, field lines are found to rotate in a circular pattern in theHMHD, whereas no such rotation is seen in the MHD results. Interestingly,plasma is also observed to be rotating in a co-spatial chromospheric region,which makes the HMHD simulation more credible. Based on the aforementionedagreements, HMHD simulation is found to agree better with observations and,thus, opens up a novel avenue to explore.

Comparison of the Hall Magnetohydrodynamics and Magnetohydrodynamics evolution of a flaring solar active region