Flare evolution and polarization changes in fine structures of solar radio emission in the 2013 April 11 event

	Flare evolution and polarization changes in fine structures of solar radio emission in the 2013 April 11 event
	Chernov, Gennady 1,2; Sych, Robert 3,4; Tan, Bao-Lin1 ; Yan, Yi-Hua1 ; Tan, Cheng-Ming1 ; Fu, Qi-Jun1 ; Karlicky, Marian 5; Fomichev, Valery 2
刊名	RESEARCH IN ASTRONOMY AND ASTROPHYSICS
	2016-02-01
卷号	16 期号:2
关键词	Sun: activity Sun: flares Sun: particle emission Sun: radio radiation zebra-pattern
英文摘要	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.
收录类别	SCI
语种	英语
WOS记录号	WOS:000369252500008
内容类型	期刊论文
源URL	[http://ir.bao.ac.cn/handle/114a11/5458]
专题	国家天文台_太阳物理研究部
作者单位	1.Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China 2.Russian Acad Sci IZMIRAN, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Troitsk 142190, Moscow Region, Russia 3.Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China 4.Russian Acad Sci, Siberian Branch, Inst Solar Terr Phys, Irkutsk 664033, Russia 5.Acad Sci Czech Republic, Inst Astron, Ondrejov 15165, Czech Republic
推荐引用方式 GB/T 7714	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.,...&Fomichev, Valery.(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).