| Name: | Samriddhi Sankar Maity |
| Affiliation: | Indian Institute of Astrophysics and Indian Institute of Science |
| Conference ID: | ASI2025_623 |
| Title: | Reconnection Flux Evolution in Erupting Magnetic Flux Ropes - perspectives from Observations and MHD Simulations |
| Authors: | Samriddhi Sankar Maity, Piyali Chatterjee, Ranadeep Sarkar, Ijas Mytheen |
| Authors Affiliation: | Samriddhi Sankar Maity (Indian Institute of Science, Bengaluru - 560012, India)
Samriddhi Sankar Maity, Piyali Chatterjee (Indian Institute of Astrophysics, Bengaluru - 560034, India)
Ranadeep Sarkar (University of Helsinki, Helsinki - 00014, Finland)
Ijas Mytheen (Amrita School of Physical Science, Kollam - 641112, India) |
| Mode of Presentation: | Oral |
| Abstract Category: | Sun, Solar System, Exoplanets, and Astrobiology |
| Abstract: | Coronal mass ejections (CMEs) are major space weather drivers, with magnetic flux ropes (MFRs) widely recognized as their primary precursors. Yet, the evolution of reconnection flux during MFR eruption remains inadequately understood. In this study, we develop a 3D magnetohydrodynamic (MHD) model to investigate the temporal evolution of reconnection flux in erupting MFRs, using both simulations and observational data. Our initial setup includes an isothermal coronal atmosphere and a potential arcade magnetic field, with an emerging MFR introduced at the lower boundary. As the MFR ascends, it stretches and compresses the overlying magnetic field, leading to the gradual formation of a current sheet and ultimately to the impulsive ejection of the flux rope. We examine the reconnection flux evolution over two consecutive MFR eruptions while continuously emerging a twisted flux rope at the lower boundary. Additionally, we analyze a similar eruptive event using observational data from the Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA). By comparing our MHD simulations with observations, we find that reconnection flux plays a key role in determining CME speeds, with a strong linear correlation between reconnection flux and MFR velocity from initiation to eruption. This simulation provides valuable insights into the complex dynamics of CME initiation and evolution. |
