A Study of Solar Radio Bursts with Fine Structures during Flare/CME Events

	A Study of Solar Radio Bursts with Fine Structures during Flare/CME Events
	Huang, J.1,2 ; Yan, Y. H.1; Liu, Y. Y.1
刊名	SOLAR PHYSICS
	2008-12-01
卷号	253 期号:1-2 页码:143-160
关键词	Radio burst Radio fine structure Solar flare CME
英文摘要	We have selected 27 solar microwave burst events recorded by the Solar Broadband Radio Spectrometer (SBRS) of China, which were accompanied by M/X class flares and fast CMEs. A total of 70.4% of radio burst events peak at 2.84 GHz before the peaks of the related flares' soft X-ray flux with an average time difference of about 6.7 minutes. Almost all of the CMEs start before or around the radio burst peaks. At 2.6 - 3.8 GHz bandwidth, 234 radio fine structures (FSs) were classified. More often, some FSs appear in groups, which can contain several individual bursts. It is found that many more radio FSs occur before the soft X-ray maxima and even before the peaks of radio bursts at 2.84 GHz. The events with high peak flux at 2.84 GHz have many more radio FSs and the durations of the radio bursts are independent of the number of radio FSs. Parameters are given for zebra patterns, type III bursts, and fiber structures, and the other types of FSs are described briefly. These radio FSs include some special types of FSs such as double type U bursts and W-type bursts.
收录类别	SCI
语种	英语
WOS记录号	WOS:000261576700010
内容类型	期刊论文
源URL	[http://ir.bao.ac.cn/handle/114a11/7389]
专题	国家天文台_太阳物理研究部
作者单位	1.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China 2.Chinese Acad Sci, Grad Univ, Beijing 100080, Peoples R China
推荐引用方式 GB/T 7714	Huang, J.,Yan, Y. H.,Liu, Y. Y.. A Study of Solar Radio Bursts with Fine Structures during Flare/CME Events[J]. SOLAR PHYSICS,2008,253(1-2):143-160.
APA	Huang, J.,Yan, Y. H.,&Liu, Y. Y..(2008).A Study of Solar Radio Bursts with Fine Structures during Flare/CME Events.SOLAR PHYSICS,253(1-2),143-160.
MLA	Huang, J.,et al."A Study of Solar Radio Bursts with Fine Structures during Flare/CME Events".SOLAR PHYSICS 253.1-2(2008):143-160.