dc.contributor.author |
Joshi, B |
|
dc.contributor.author |
Mitra, P. K |
|
dc.contributor.author |
Bhattacharyya, R |
|
dc.contributor.author |
Upadhyay, K |
|
dc.contributor.author |
Oberoi, Divya |
|
dc.contributor.author |
Sasikumar Raja, K |
|
dc.contributor.author |
Monstein, Christian |
|
dc.date.accessioned |
2021-07-16T05:37:01Z |
|
dc.date.available |
2021-07-16T05:37:01Z |
|
dc.date.issued |
2021-06 |
|
dc.identifier.citation |
Solar Physics, Vol. 296, No. 6, 85 |
en_US |
dc.identifier.issn |
1573-093X |
|
dc.identifier.uri |
http://hdl.handle.net/2248/7782 |
|
dc.description |
Restricted Access |
en_US |
dc.description |
The original publication is available at springerlink.com |
|
dc.description.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 (≈50--180 MHz), stationary plasma emission for ≈7 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 ≈2.5 MHz precedes the stationary type IV burst observed by Udaipur-CALLISTO by ≈5 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. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
Springer |
en_US |
dc.relation.uri |
https://doi.org/10.1007/s11207-021-01820-6 |
|
dc.rights |
© Springer |
|
dc.subject |
Solar flares |
en_US |
dc.subject |
Long Duration Event (LDE) |
en_US |
dc.subject |
Magnetic reconnection |
en_US |
dc.subject |
Solar radio bursts |
en_US |
dc.title |
Two-stage evolution of an extended C-class eruptive flaring activity from sigmoid active region NOAA 12734: SDO and Udaipur-CALLISTO observations |
en_US |
dc.type |
Article |
en_US |