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Title: INITIATION PROCESSES FOR THE 2013 MAY 13 X1.7 LIMB FLARE

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 ofmore » magnetic reconnection between sheared magnetic fields that also produced the MFR.« less

Authors:
 [1]; ; ;  [2]
  1. Xinjiang Astronomical Observatory, CAS, 830011, Urumqi (China)
  2. Purple Mountain Observatory, CAS, Nanjing, 210008 (China)
Publication Date:
OSTI Identifier:
22663998
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 835; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; EXPANSION; EXTREME ULTRAVIOLET RADIATION; LIMBS; MAGNETIC CORES; MAGNETIC FIELDS; MAGNETIC FLUX; MAGNETIC RECONNECTION; SUN; SUNSPOTS; X RADIATION

Citation Formats

Shen, Jinhua, Wang, Ya, Zhou, Tuanhui, and Ji, Haisheng. INITIATION PROCESSES FOR THE 2013 MAY 13 X1.7 LIMB FLARE. United States: N. p., 2017. Web. doi:10.3847/1538-4357/835/1/43.
Shen, Jinhua, Wang, Ya, Zhou, Tuanhui, & Ji, Haisheng. INITIATION PROCESSES FOR THE 2013 MAY 13 X1.7 LIMB FLARE. United States. doi:10.3847/1538-4357/835/1/43.
Shen, Jinhua, Wang, Ya, Zhou, Tuanhui, and Ji, Haisheng. Fri . "INITIATION PROCESSES FOR THE 2013 MAY 13 X1.7 LIMB FLARE". United States. doi:10.3847/1538-4357/835/1/43.
@article{osti_22663998,
title = {INITIATION PROCESSES FOR THE 2013 MAY 13 X1.7 LIMB FLARE},
author = {Shen, Jinhua and Wang, Ya and Zhou, Tuanhui and Ji, Haisheng},
abstractNote = {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.},
doi = {10.3847/1538-4357/835/1/43},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 835,
place = {United States},
year = {2017},
month = {1}
}