YNAO OpenIR  > 抚仙湖太阳观测和研究基地
Downfiow-induced brightening following a filament eruption
Xue ZK(薛志科)1,3; Yan XL(闫晓理)1,2; Qu ZQ(屈中权)1; Zhao, L4
发表期刊NEW ASTRONOMY
2014-01
卷号26页码:23-32
DOI10.1016/j.newast.2013.04.005
产权排序第1完成单位
收录类别SCI
关键词Sun: Filaments Sun: Activity Sun: Magnetic Fields Sun: Oscillations Sun: Corona
摘要

The plasma from solar filament eruptions sometimes falls down to the lower solar atmosphere. These interesting events can help us to understand the properties of downflows, such as the temperature and the conversion between kinetic energy and thermal energy. We analyze the case of a filament eruption in active region NOAA 11283 and brightening caused by the return of filament material on September 7 and 8, 2014, observed by the Atmospheric Imaging Assembly (ALA) and the Helioseismic and Magnetic Imager (HMI) aboard the Solar Dynamics Observatory (SDO). Magnetic flux cancellation was observed as a result of the eruption after the eruptive filament started to ascend. Another filament near the eruptive filament was disturbed by an extreme ultraviolet (EUV) wave that was triggered by the eruptive filament, causing it to oscillate. Based on coronal seismology, the mean magnetic field strength in the oscillatory filament was estimated to be approximately 18 +/- 2 G. Some plasma separated from the filament and fell down to the solar northwest surface after the filament eruption. The velocities of the downflows increased at accelerations lower than the gravitational acceleration. The main characteristic temperature of the downflows was about 5 x 10(4) K. When the plasma blobs fell down to lower atmospheric heights, the high-speed downward-travelling plasma collided with plasma at lower atmospheric heights, causing the plasma to brighten. The brightening was observed in all 8 AIA channels, demonstrating that the temperature of the plasma in the brightening covered a wide range of values, from 10(5) K to 10(7) K. This brightening indicates the conversion between kinetic energy and thermal energy. (C) 2013 Elsevier B.V. All rights reserved.

资助项目National Science Foundation of China (NSFC)[10903027] ; National Science Foundation of China (NSFC)[11078005] ; National Science Foundation of China (NSFC)[10943002] ; National Science Foundation of China (NSFC)[11103075] ; Key Laboratory of Solar Activity of CAS[KLSA201220] ; China's 973 project[G2011CB811400]
项目资助者National Science Foundation of China (NSFC)[10903027, 11078005, 10943002, 11103075] ; Key Laboratory of Solar Activity of CAS[KLSA201220] ; China's 973 project[G2011CB811400]
语种英语
学科领域天文学 ; 太阳与太阳系 ; 太阳物理学
学科门类理学 ; 理学::天文学
文章类型Article
出版者ELSEVIER SCIENCE BV
出版地PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
ISSN1384-1076
URL查看原文
归档日期2013-10-21
WOS记录号WOS:000325510600003
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]CORONAL MASS EJECTIONS ; LOOP OSCILLATIONS ; TRANSVERSE OSCILLATIONS ; MAGNETIC-FIELD ; SOLAR-FLARES ; EIT WAVES ; HEATING MECHANISMS ; TRANSITION-REGION ; PROMINENCE ; DOWNFLOW
引用统计
被引频次:8[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/4710
专题抚仙湖太阳观测和研究基地
通讯作者Xue ZK(薛志科)
作者单位1.National Astronomical Observatories of China/Yunnan Astronomical Observatory, Chinese Academy of Sciences, Kunming, Yunnan 650011, China
2.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
3.University of Chinese Academy of Sciences, Beijing 100049, China
4.Yunnan Normal University, Kunming 650092, China
第一作者单位中国科学院云南天文台
通讯作者单位中国科学院云南天文台
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GB/T 7714
Xue ZK,Yan XL,Qu ZQ,et al. Downfiow-induced brightening following a filament eruption[J]. NEW ASTRONOMY,2014,26:23-32.
APA Xue ZK,Yan XL,Qu ZQ,&Zhao, L.(2014).Downfiow-induced brightening following a filament eruption.NEW ASTRONOMY,26,23-32.
MLA Xue ZK,et al."Downfiow-induced brightening following a filament eruption".NEW ASTRONOMY 26(2014):23-32.
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