Large-scale contraction and subsequent disruption of coronal loops during various phases of the M6.2 flare associated with the confined flux rope eruption

Show simple item record

dc.contributor.author Kushwaha, Upendra Kumar Singh
dc.contributor.author Joshi, Bhuwan
dc.contributor.author Veronig, Astrid M.
dc.contributor.author Moon, Yong-Jae
dc.date.accessioned 2015-04-26T17:26:01Z
dc.date.available 2015-04-26T17:26:01Z
dc.date.issued 2015-04
dc.identifier.citation Kushwaha, Upendra; Joshi, Bhuwan; Veronig, Astrid M. and Moon, Yong-Jae, “Large-scale contraction and subsequent disruption of coronal loops during various phases of the M6.2 flare associated with the confined flux rope eruption”, arXiv, Cornell University Library, DOI: arXiv:1504.01888, Apr. 2015. en_US
dc.identifier.uri https://repository.iitgn.ac.in/handle/123456789/1713
dc.description.abstract We present a detailed multi-wavelength study of the M6.2 flare which was associated with a confined eruption of a prominence using TRACE, RHESSI, and NoRH observations. The pre-flare phase of this event is characterized by spectacular large-scale contraction of overlying extreme ultraviolet (EUV) coronal loops during which the loop system was subjected to an altitude decrease of ~20 Mm for an extended span of ~30 min. This contraction phase is accompanied by sequential EUV brightenings associated with hard X-ray (HXR) (up to 25 keV) and microwave (MW) sources from low-lying loops in the core of the flaring region which together with X-ray spectra indicate strong localized heating in the source region before the filament activation and associated M-class flare. With the onset of the impulsive phase of the M6.2 flare, we detect HXR and MW sources that exhibit intricate temporal and spatial evolution in relation with the fast rise of the prominence. Following the flare maximum, the filament eruption slowed down and subsequently confined within the large overlying active region loops; the event did not lead to a coronal mass ejection (CME). During the confinement process of the erupting prominence, we detect MW emission from the extended coronal region with multiple emission centroids which likely represent emission from hot blobs of plasma formed after the collapse of the expanding flux rope and entailing prominence material. RHESSI observations reveal high plasma temperature (~30 MK) and substantial non-thermal characteristics with electron spectral index (~5) during the impulsive phase of the flare. The time-evolution of thermal energy exhibits a good correspondence with the variations in cumulative non-thermal energy which suggest that the energy of accelerated particles efficiently converted to hot flare plasma implying an effective validation of the Neupert effect. en_US
dc.description.statementofresponsibility by Upendra Kushwaha, et al
dc.language.iso en en_US
dc.publisher Cornell University Library en_US
dc.subject Multi-wavelength en_US
dc.subject RHESSI en_US
dc.subject NoRH observations en_US
dc.subject Pre-flare phase en_US
dc.title Large-scale contraction and subsequent disruption of coronal loops during various phases of the M6.2 flare associated with the confined flux rope eruption en_US
dc.type Presentation en_US


Files in this item

Files Size Format View

There are no files associated with this item.

This item appears in the following Collection(s)

Show simple item record

Search Digital Repository


Browse

My Account