Abstract
In this article, we present a multi-wavelength investigation of a C-class flaring activity that occurred in the active region NOAA 12734 on 8 March 2019. The investigation utilizes data from the Atmospheric Imaging Assembly (AIA) and the Helioseismic Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) and the Udaipur-CALLISTO solar radio spectrograph of the Physical Research Laboratory. This low intensity C1.3 event is characterized by typical features of a long-duration event (LDE), viz. extended flare arcade, large-scale two-ribbon structures and twin coronal dimmings. The eruptive event occurred in a coronal sigmoid and displayed two distinct stages of energy release, manifested in terms of temporal and spatial evolution. The formation of twin-dimming regions are consistent with the eruption of a large flux rope with footpoints lying in the western and eastern edges of the coronal sigmoid. The metric radio observations obtained from Udaipur-CALLISTO reveals a broad-band (\(\approx50\,\text{--}\,180~\text{MHz}\)), stationary plasma emission for \(\approx7~\text{min}\) during the second stage of the flaring activity that resemble a type IV radio burst. A type III decametre-hectometre radio bursts with starting frequency of \(\approx2.5~\text{MHz}\) precedes the stationary type IV burst observed by Udaipur-CALLISTO by \(\approx5~\text{min}\). The synthesis of multi-wavelength observations and non-linear force-free field (NLFFF) coronal modeling together with magnetic decay index analysis suggest that the sigmoid flux rope underwent a zipping-like uprooting from its western to eastern footpoints in response to the overlying asymmetric magnetic field confinement. The asymmetrical eruption of the flux rope also accounts for the observed large-scale structures viz. apparent eastward shift of flare ribbons and post-flare loops along the polarity inversion line (PIL), and provides evidence for lateral progression of magnetic reconnection site as the eruption proceeds.
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Notes
At a distance of 1 AU, an angular diameter of 1 arcsec represents \(\approx0.725~\text{Mm}\) on the Sun. As a standard assumption, this conversion factor is uniformly applied across the whole magnetogram.
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Acknowledgements
We are grateful to Dr. Anil Bhardwaj, Director, Physical Research Laboratory, Ahmedahad, India for his encouragement and support toward CALLISTO project at USO/PRL. We also sincerely thank Dr. Yashwant Gupta, Centre Director, NCRA-TIFR, Pune, India for providing technical expertise and facilities to fabricate the LPDA. We thank the SDO and GOES teams for their open data policy. SDO is NASA’s missions under the Living With a Star (LWS) program. We also thank FHNW, Institute for Data Science in Brugg/Windisch, Switzerland for hosting the e-Callisto network. DO acknowledges support of the Department of Atomic Energy, Government of India, under the project no. 12-R&D-TFR-5.02-0700. We thank Dr. Thomas Wiegelmann for providing the NLFFF code. We are also thankful to Binal Patel for help in the analysis of the radio spectrum. We are grateful to the referee of the paper for providing us with a very constructive set of comments and suggestions that enhanced the scientific content and presentation of the paper.
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Joshi, B., Mitra, P.K., Bhattacharyya, R. et al. Two-Stage Evolution of an Extended C-Class Eruptive Flaring Activity from Sigmoid Active Region NOAA 12734: SDO and Udaipur-CALLISTO Observations. Sol Phys 296, 85 (2021). https://doi.org/10.1007/s11207-021-01820-6
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DOI: https://doi.org/10.1007/s11207-021-01820-6