TY - JOUR
T1 - Statistical Study of Magnetic Topology for Eruptive and Confined Solar Flares
AU - Cui, Yanmei
AU - Wang, Haimin
AU - Xu, Yan
AU - Liu, Siqing
N1 - Funding Information:
We thank the referees for their valu able comments. We acknowledge the use of the solar data from the LASCO, EIT, and MDI instruments on board the SOHO spacecraft, from the HMI and AIA instruments on board the SDO spacecraft, and from GOES sys tem. The CME catalog is generated and maintained at the CDAW Data Center by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. The solar flare reports are compiled by the Space Weather Prediction Center of NOAA. Yanmei Cui and Siqing Liu are supported by grants from National Natural Science Foundation of China (41604149). Yan Xu and Haimin Wang acknowl edge supports from U.S. NSF under grants AGS-1408703, AGS-1539791, and AGS-1620875.
Publisher Copyright:
©2018. American Geophysical Union. All Rights Reserved.
PY - 2018/3
Y1 - 2018/3
N2 - Large flares and halo coronal mass ejections (CMEs) can often cause strong space environment disturbances and sequently a series of space environment effects. The X-class flares associated with halo CMEs are particular prone to these effects. In this paper, 58 X-class flares were collected and studied with the source locations in 30° from the disk center, which were observed from 1996 to 2015. Among these events, 48 flares were associated with CMEs and defined as “eruptive” events. The other 10 flares without CMEs were defined as “confined” flares. By comparing the properties of flares and associated magnetic fields for the two sets of samples, we found the following: (1) magnetic free energy and overlying transverse fields play important roles in producing solar eruptions. Eruptive flares with high-speed CMEs tend to occur in active regions with more free energy and larger decay index. (2) CME speeds are affected by magnetic free energy, which are described by parameters of the unsigned magnetic flux, the area of polarity inversion region, and the strength of transverse fields in the low altitude. These parameters have moderate positive correlations with CME speeds.
AB - Large flares and halo coronal mass ejections (CMEs) can often cause strong space environment disturbances and sequently a series of space environment effects. The X-class flares associated with halo CMEs are particular prone to these effects. In this paper, 58 X-class flares were collected and studied with the source locations in 30° from the disk center, which were observed from 1996 to 2015. Among these events, 48 flares were associated with CMEs and defined as “eruptive” events. The other 10 flares without CMEs were defined as “confined” flares. By comparing the properties of flares and associated magnetic fields for the two sets of samples, we found the following: (1) magnetic free energy and overlying transverse fields play important roles in producing solar eruptions. Eruptive flares with high-speed CMEs tend to occur in active regions with more free energy and larger decay index. (2) CME speeds are affected by magnetic free energy, which are described by parameters of the unsigned magnetic flux, the area of polarity inversion region, and the strength of transverse fields in the low altitude. These parameters have moderate positive correlations with CME speeds.
KW - Confined flares
KW - Eruptive flares
KW - Magnetic topology
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U2 - 10.1002/2017JA024710
DO - 10.1002/2017JA024710
M3 - Article
AN - SCOPUS:85043373607
SN - 2169-9380
VL - 123
SP - 1704
EP - 1714
JO - Journal of Geophysical Research: Space Physics
JF - Journal of Geophysical Research: Space Physics
IS - 3
ER -