Detailed analysis of dynamic evolution of three Active Regions at the photospheric level before flare and CME occurrence

	Detailed analysis of dynamic evolution of three Active Regions at the photospheric level before flare and CME occurrence
	Ye Yudong; Korsós M.B.; Erdélyi R.; Korsós, M.B. (korsos.marianna@csfk.mta.hu)
刊名	Advances in Space Research
	2017
ISSN号	0273-1177
英文摘要	We present a combined analysis of the applications of the weighted horizontal magnetic gradient (denoted as WGM in Korsós et al. (2015)) method and the magnetic helicity tool (Berger and Field, 1984) employed for three active regions (ARs), namely NOAA AR 11261, AR 11283 and AR 11429. We analysed the time series of photospheric data from the Solar Dynamics Observatory taken between August 2011 and March 2012. During this period the three ARs produced a series of flares (eight M- and six X-class) and coronal mass ejections (CMEs). AR 11261 had four M-class flares and one of them was accompanied by a fast CME. AR 11283 had similar activities with two M- and two X-class flares, but only with a slow CME. Finally, AR 11429 was the most powerful of the three ARs as it hosted five compact and large solar flare and CME eruptions. For applying the WGM method we employed the Debrecen sunspot data catalogue, and, for estimating the magnetic helicity at photospheric level we used the Space-weather HMI Active Region Patches (SHARP's) vector magnetograms from SDO/HMI (Solar Dynamics Observatory/Helioseismic and Magnetic Imager). We followed the evolution of the components of the WGM and the magnetic helicity before the flare and CME occurrences. We found a unique and mutually shared behaviour, called the U-shaped pattern, of the weighted distance component of WGM and of the shearing component of the helicity flux before the flare and CME eruptions. This common pattern is associated with the decreasing-receding phases yet reported only known to be a necessary feature prior to solar flare eruption(s) but found now at the same time in the evolution of the shearing helicity flux. This result leads to the conclusions that (i) the shearing motion of photospheric magnetic field may be a key driver for solar eruption in addition to the flux emerging process, and that (ii) the found decreasing-approaching pattern in the evolution of shearing helicity flux may be another precursor indicator for improving the forecasting of solar eruptions. © 2017.
语种	英语
内容类型	期刊论文
源URL	[http://ir.nssc.ac.cn/handle/122/6073]
专题	国家空间科学中心_空间科学部
通讯作者	Korsós, M.B. (korsos.marianna@csfk.mta.hu)
推荐引用方式 GB/T 7714	Ye Yudong,Korsós M.B.,Erdélyi R.,et al. Detailed analysis of dynamic evolution of three Active Regions at the photospheric level before flare and CME occurrence[J]. Advances in Space Research,2017.
APA	Ye Yudong,Korsós M.B.,Erdélyi R.,&Korsós, M.B. .(2017).Detailed analysis of dynamic evolution of three Active Regions at the photospheric level before flare and CME occurrence.Advances in Space Research.
MLA	Ye Yudong,et al."Detailed analysis of dynamic evolution of three Active Regions at the photospheric level before flare and CME occurrence".Advances in Space Research (2017).