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Flare evolution and polarization changes in fine structures of solar radio emission in the 2013 April 11 event
Chernov, Gennady1,2; Sych, Robert3,4; Tan, Bao-Lin1; Yan, Yi-Hua1; Tan, Cheng-Ming1; Fu, Qi-Jun1; Karlicky, Marian5; Fomichev, Valery2; Chernov, G (reprint author), Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China
发表期刊RESEARCH IN ASTRONOMY AND ASTROPHYSICS
2016-02-01
卷号16期号:2
DOI10.1088/1674-4527/16/2/028
产权排序第3完成单位
收录类别SCI
关键词Sun: Activity Sun: Flares Sun: Particle Emission Sun: Radio Radiation Zebra-pattern
摘要The measurement of positions and sizes of radio sources in observations is important for understanding of the flare evolution. For the first time, solar radio spectral fine structures in an M6.5 flare that occurred on 2013 April 11 were observed simultaneously by several radio instruments at four different observatories: Chinese Solar Broadband Radio Spectrometer at Huairou (SBRS/Huairou), Ondrejov Radio Spectrograph in the Czech Republic (ORSC/Ondrejov), Badary Broadband Microwave Spectropolarimeter (BMS/Irkutsk), and spectrograph/IZMIRAN (Moscow, Troitsk). The fine structures included microwave zebra patterns (ZPs), fast pulsations and fiber bursts. They were observed during the flare brightening located at the tops of a loop arcade as shown in images taken by the extreme ultraviolet (EUV) telescope onboard NASA's satellite Solar Dynamics Observatory (SDO). The flare occurred at 06:58-07:26 UT in solar active region NOAA 11719 located close to the solar disk center. ZPs appeared near high frequency boundaries of the pulsations, and their spectra observed in Huairou and Ondrejov agreed with each other in terms of details. At the beginning of the flare's impulsive phase, a strong narrowband ZP burst occurred with a moderate left-handed circular polarization. Then a series of pulsations and ZPs were observed in almost unpolarized emission. After 07:00 UT a ZP appeared with a moderate right-handed polarization. In the flare decay phase (at about 07:25 UT), ZPs and fiber bursts become strongly right-hand polarized. BMS/Irkutsk spectral observations indicated that the background emission showed a left-handed circular polarization (similar to SBRS/Huairou spectra around 3 GHz). However, the fine structure appeared in the right-handed polarization. The dynamics of the polarization was associated with the motion of the flare exciter, which was observed in EUV images at 171 angstrom and 131 angstrom by the SDO Atmospheric Imaging Assembly (AIA). Combining magnetograms observed by the SDO Helioseismic and Magnetic Imager (HMI) with the homologous assumption of EUV flare brightenings and ZP bursts, we deduced that the observed ZPs correspond to the ordinary radio emission mode. However, future analysis needs to verify the assumption that zebra radio sources are really related to a closed magnetic loop, and are located at lower heights in the solar atmosphere than the source of pulsations.
项目资助者Chinese Academy of Sciences Visiting Professorship for Senior International Scientists(2011T1J20) ; Chinese Academy of Sciences President's International Fellowship Initiative(2015VMA014) ; Russian Foundation for Basic Research (13-02-00044, 13-02-90472, 14-02-91157, 14-02-00367) ; National Natural Science Foundation of China (11273030, 11103044, 11103039, 11221063, 11373039, 113111042) ; MOST(2011CB811401) ; National Major Scientific Equipment RD Project(ZDYZ 2009-3, P209/12/00103 GA CR)
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN1674-4527
URL查看原文
WOS记录号WOS:000369252500008
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]CYCLOTRON WAVE INSTABILITY ; ZEBRA-PATTERN ; BURSTS ; ORIGIN ; CORONA ; SPECTROMETER ; DYNAMICS ; STRIPES
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被引频次:1[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/114a53/9330
专题射电天文研究组
通讯作者Chernov, G (reprint author), Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China
作者单位1.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
2.Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Russian Academy of Sciences (IZMIRAN), Troitsk, Moscow region, 142190, Russia
3.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China
4.Institute of Solar-Terrestrial Physics, Russian Academy of Sciences, Siberian Branch, Irkutsk 664033, Russia
5.Astronomical Institute of the Academy of Sciences of the Czech Republic, Ondrejov 15165, Czech Republic
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Chernov, Gennady,Sych, Robert,Tan, Bao-Lin,et al. Flare evolution and polarization changes in fine structures of solar radio emission in the 2013 April 11 event[J]. RESEARCH IN ASTRONOMY AND ASTROPHYSICS,2016,16(2).
APA Chernov, Gennady.,Sych, Robert.,Tan, Bao-Lin.,Yan, Yi-Hua.,Tan, Cheng-Ming.,...&Chernov, G .(2016).Flare evolution and polarization changes in fine structures of solar radio emission in the 2013 April 11 event.RESEARCH IN ASTRONOMY AND ASTROPHYSICS,16(2).
MLA Chernov, Gennady,et al."Flare evolution and polarization changes in fine structures of solar radio emission in the 2013 April 11 event".RESEARCH IN ASTRONOMY AND ASTROPHYSICS 16.2(2016).
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