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Author Shen, Jinhua ♦ Wang, Ya ♦ Zhou, Tuanhui ♦ Ji, Haisheng
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ EXPANSION ♦ EXTREME ULTRAVIOLET RADIATION ♦ LIMBS ♦ MAGNETIC CORES ♦ MAGNETIC FIELDS ♦ MAGNETIC FLUX ♦ MAGNETIC RECONNECTION ♦ SUN ♦ SUNSPOTS ♦ X RADIATION
Abstract For the X1.7 class flare on 2013 May 13 (SOL2013-05-13T01:53), its initiation process was well observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory and the Extreme UltraViolet Imager (EUVI) on board STEREO-B . The initiation process incorporates the following phenomena: an X-ray precursor that started ∼9 minutes before flare onset, two hot magnetic loops (as seen with AIA hot channels) forming a sigmoidal core magnetic structure (as seen with the EUVI), a rapidly formed magnetic flux rope (MFR) that expands outward, and a flare loop that contracts inward. The two hot magnetic loops were activated after the occurrence of the X-ray precursor. After activation, magnetic reconnection occurred between the two hot magnetic loops (inside the sigmoid structure), which produced the expanding MFR and the contracting flare loop (CFL). The MFR and CFL can only be seen with AIA hot and cool channels, respectively. For this flare, the real initiation time can be regarded as being from the starting time of the precursor, and its impulsive phase started when the MFR began its fast expansion. In addition, the CFL and the growing postflare magnetic loops are different loop systems, and the CFL was the product of magnetic reconnection between sheared magnetic fields that also produced the MFR.
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 2017-01-20
Publisher Place United States
Journal Astrophysical Journal
Volume Number 835
Issue Number 1


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