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Magnetic structure of solar flare regions producing hard X-ray pulsations
Zimovets, I., V; Wang, R.; Liu, Y. D.; Wang, C.; Kuznetsov, S. A.; Sharykin, I. N.; Struminsky, A. R.; Nakariakov, V. M.; Zimovets, IV (reprint author), Natl Space Sci Ctr CAS, Int Space Sci Inst Beijing, 1 Nanertiao, Beijing 100190, Peoples R China.
作者部门空间科学部
发表期刊JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
2018
卷号174页码:17-27
ISSN1364-6826
语种英语
关键词Solar Flares Magnetic Field Magnetic Flux Rope Hard X-ray Pulsations
摘要We present analysis of the magnetic field in seven solar flare regions accompanied by the pulsations of hard Xray (HXR) emission. These flares were studied by Kuznetsov et al. (2016) (Paper I), and chosen here because of the availability of the vector magnetograms for their parent active regions (ARs) obtained with the SDO/HMI data. In Paper I, based on the observations only, it was suggested that a magnetic flux rope (MFR) might play an important role in the process of generation of the HXR pulsations. The goal of the present paper is to test this hypothesis by using the extrapolation of magnetic field with the non-linear force-free field (NLFFF) method. Having done this, we found that before each flare indeed there was an MFR elongated along and above a magnetic polarity inversion line (MPIL) on the photosphere. In two flare regions the sources of the HXR pulsations were located at the footpoints of different magnetic field lines wrapping around the central axis, and constituting an MFR by themselves. In five other flares the parent field lines of the HXR pulsations were not a part of an MFR, but surrounded it in the form of an arcade of magnetic loops. These results show that, at least in the analyzed cases, the "single flare loop" models do not satisfy the observations and magnetic field modeling, while are consistent with the concept that the HXR pulsations are a consequence of successive episodes of energy release and electron acceleration in different magnetic flux tubes (loops) of a complex AR. An MFR could generate HXR pulsations by triggering episodes of magnetic reconnection in different loops in the course of its non-uniform evolution along an MPIL. However, since three events studied here were confined flares, actual eruptions may not be required to trigger sequential particle acceleration episodes in the magnetic systems containing an MFR.
收录类别SCI
文献类型期刊论文
条目标识符http://ir.nssc.ac.cn/handle/122/6354
专题空间科学部
通讯作者Zimovets, IV (reprint author), Natl Space Sci Ctr CAS, Int Space Sci Inst Beijing, 1 Nanertiao, Beijing 100190, Peoples R China.
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GB/T 7714
Zimovets, I., V,Wang, R.,Liu, Y. D.,et al. Magnetic structure of solar flare regions producing hard X-ray pulsations[J]. JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS,2018,174:17-27.
APA Zimovets, I., V.,Wang, R..,Liu, Y. D..,Wang, C..,Kuznetsov, S. A..,...&Zimovets, IV .(2018).Magnetic structure of solar flare regions producing hard X-ray pulsations.JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS,174,17-27.
MLA Zimovets, I., V,et al."Magnetic structure of solar flare regions producing hard X-ray pulsations".JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 174(2018):17-27.
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