TY - JOUR
T1 - Re-flaring of a post-flare loop system driven by flux rope emergence and twisting
AU - Cheng, X.
AU - Ding, M. D.
AU - Guo, Y.
AU - Zhang, J.
AU - Jing, Ju
AU - Wiegelmann, T.
N1 - Copyright:
Copyright 2015 Elsevier B.V., All rights reserved.
PY - 2010
Y1 - 2010
N2 - In this Letter, we study in detail the evolution of the post-flare loops on 2005 January 15 that occurred between two consecutive solar eruption events, both of which generated a fast halo coronal mass ejection (CME) and a major flare. The post-flare loop system, formed after the first CME/flare eruption, evolved rapidly, as manifested by the unusual accelerating rise motion of the loops. Through nonlinear force-free field models, we obtain the magnetic structure over the active region. It clearly shows that the flux rope below the loops also kept rising, accompanied with increasing twist and length. Finally, the post-flare magnetic configuration evolved to a state that resulted in the second CME/flare eruption. This is an event in which the post-flare loops can re-flare in a short period of ∼ 16 hr following the first CME/flare eruption. The observed re-flaring at the same location is likely driven by the rapid evolution of the flux rope caused by the magnetic flux emergence and the rotation of the sunspot. This observation provides valuable information on CME/flare models and their prediction.
AB - In this Letter, we study in detail the evolution of the post-flare loops on 2005 January 15 that occurred between two consecutive solar eruption events, both of which generated a fast halo coronal mass ejection (CME) and a major flare. The post-flare loop system, formed after the first CME/flare eruption, evolved rapidly, as manifested by the unusual accelerating rise motion of the loops. Through nonlinear force-free field models, we obtain the magnetic structure over the active region. It clearly shows that the flux rope below the loops also kept rising, accompanied with increasing twist and length. Finally, the post-flare magnetic configuration evolved to a state that resulted in the second CME/flare eruption. This is an event in which the post-flare loops can re-flare in a short period of ∼ 16 hr following the first CME/flare eruption. The observed re-flaring at the same location is likely driven by the rapid evolution of the flux rope caused by the magnetic flux emergence and the rotation of the sunspot. This observation provides valuable information on CME/flare models and their prediction.
KW - Sun: corona
KW - Sun: coronal mass ejections (CMEs)
KW - Sun: flares
KW - Sun: magnetic topology
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U2 - 10.1088/2041-8205/716/1/L68
DO - 10.1088/2041-8205/716/1/L68
M3 - Article
AN - SCOPUS:77952945225
VL - 716
SP - L68-L73
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 1 PART 2
ER -