NDLI: Radio evidence for breakout reconnection in solar eruptive events

Content Provider	EDP Sciences
Author	H. Aurass G. Holman S. Braune G. Mann P. Zlobec
Abstract	Context. Magnetic reconnection is understood to be fundamental to energy release in solar eruptive events (SEEs). In these events reconnection produces a magnetic flux rope above an arcade of hot flare loops. Breakout reconnection, a secondary reconnection high in the corona between this flux rope and the overlying magnetic field, has been hypothesized. Direct observational evidence for breakout reconnection has been elusive, however.Aims. The aim of this study is to establish a plausible interpretation of the combined radio and hard X-ray (HXR) emissions observed during the impulsive phase of the near-limb X3.9-class SEE on 2003 November 03.Methods. We study radio spectra (AIP), simultaneous radio images (Nançay Multi-frequency Radio Heliograph, NRH), and single-frequency polarimeter data (OAT). The radio emission is nonthermal plasma radiation with a complex structure in frequency and time. Emphasis is on the time interval when the HXR flare loop height was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI) to be at its minimum and an X-ray source was observed above the top of the arcade loops.Results. Two stationary, meter-wavelength sources are observed radially aligned at 0.18 and 0.41 R_{⊙_{above the active region and HXR sources. The lower source is apparently associated with the upper reconnection jet of the flare current sheet (CS), and the upper source is apparently associated with breakout reconnection. Sources observed at lower radio frequencies surround the upper source at the expected locations of the breakout reconnection jets.Conclusions. We believe the upper radio source is the most compelling evidence to date for the onset of breakout reconnection during a SEE. The height stationarity of the breakout sources and their dynamic radio spectrum discriminate them from propagating disturbances. Timing and location arguments reveal for the first time that both the earlier described above the flare loop top HXR source and the lower radio source are emission from the upper reconnection jet above the vertical flare CS.}}
Page Count	8
File Format	HTM / HTML PDF
ISSN	00046361
Alternate Webpage(s)	https://www.aanda.org/articles/aa/abs/2013/07/aa21111-13/aa21111-13.html
e-ISSN	14320746
Journal	Astronomy & Astrophysics
Volume Number	555
DOI	10.1051/0004-6361/201321111
Language	English
Publisher	EDP Sciences
Publisher Date	2013-07-01
Access Restriction	Open
Rights Holder	© ESO, 2013
Subject Keyword	Sun: radio radiation Sun: X-rays, gamma rays Sun: coronal mass ejections (CMEs) Sun: magnetic topology Sun: flares Sun: corona Sun: radio radiation / Sun: X-rays, gamma rays / Sun: coronal mass ejections (CMEs) / Sun: magnetic topology / Sun: flares / Sun: corona
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science

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1	Ministry of Education (GoI), Department of Higher Education	Sanctioning Authority	https://www.education.gov.in/ict-initiatives
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3	National Digital Library of India Office, Indian Institute of Technology Kharagpur	The administrative and infrastructural headquarters of the project	Dr. B. Sutradhar bsutra@ndl.gov.in
4	Project PI / Joint PI	Principal Investigator and Joint Principal Investigators of the project	Dr. B. Sutradhar bsutra@ndl.gov.in Prof. Saswat Chakrabarti will be added soon
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