| Name: | Sushree Sangeeta Nayak |
| Affiliation: | Center for Space Plasma and Aeronomic Research |
| Conference ID: | ASI2025_418 |
| Title: | flare ribbon dynamics using MHD simulation |
| Authors: | Sushree S Nayak(1), Qiang Hu (1,2), Wen He (1), Sanjay Kumar (3), & R Bhattacharyya (4) |
| Authors Affiliation: | 1) Center for Space Plasma and Aeronomic Research, the University of Alabama in Huntsville, AL
2) Dept. of Space Science, the University of Alabama in Huntsville, AL
3) Patna University, Patna, IN
4) Udaipur Solar Observatory, Physical Research Laboratory, Rajasthan, IN |
| Mode of Presentation: | Oral |
| Abstract Category: | Sun, Solar System, Exoplanets, and Astrobiology |
| Abstract: | We have studied the properties of magnetic reconnection through flare ribbons dynamics using observations and data-constrained magnetohydrodynamics (MHD) simulation. We have estimated the reconnection flux and reconnection flux rates using flare ribbons observed in 1600 channel in Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) of an M1.1 flare hosted by the active region 12184 on May 23, 2021 utilizing the technique developed by Qiu et al 2006. We find the reconnection flux and corresponding flux rates to be $10^{20}$ Mx and flux rate $10^{18}$ Mx/s respectively. To understand the origin of flare ribbons, we have performed an MHD simulation initiated by the non-force-free-field extrapolated field. Importantly, we have identified a three-dimensional (3D) magnetic neutral point and a flux rope in the flaring region, which are crucial to the flaring activity. The reconnection initiates at the null point. Later, the flux rope appears to reconnect at the null, which is favorable for the eruption of the filament. We trace the footpoint evolution of the field lines lying over the flare ribbons and find a significant matching between the observed flare ribbons and the evolution of footpoints computed from the MHD simulation. From the simulation, we have calculated the reconnection flux and flux rates using the pixels under these footpoints and found one order higher in comparison to their observed values. Interesting is also the enhancement of vertical current density near the flaring ribbons, a signature of successive reconnections near the null point. This is again completed by the presence of high squashing factor in the vicinity of ribbons indicating slipping reconnections of the fan field lines of the null skeleton over the ribbons. The findings from the simulation contribute toward the understandings of ribbon formation in a flaring process as well as involved magnetic reconnection.
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