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Microwave type III bursts and pulsation groups
Ning, Z; Ding, MD; Wu, HA; Xu, FY; Meng, X
刊名ASTRONOMY & ASTROPHYSICS
2005-07-01
卷号437期号:2页码:691-697
关键词Sun : radio radiation
ISSN号0004-6361
英文摘要We analyse 22 continuous microwave reverse slope (RS) type III and 21 microwave pulsation groups observed by the Purple Mountain Observatory (PMO) spectrometer over the frequency range of 4.5-7.5 GHz from 1999-2003. The RS type III groups have an average of 12 bursts per group, a mean duration of 0.1-2 s around 6 GHz, a mean quasi-period of 2.0 +/- 0.6 s and a mean drift rate of 7.0 GHz s(-1). The shortest quasi-period is measurable down to 0.05 s thanks to the high time resolution of this instrument. The microwave pulsation groups have an average of 22 events per group, a mean duration of 3-4 s and a mean quasi-period of 3.7 +/- 1.1 s. The RS type III bursts have the same quasi-period as the upward type III bursts documented before. We discuss two possible origins of the quasi-periodicity of type III bursts. One is the quasi-periodic process in magnetic reconnection at the same site, and the other is spatially unresolved stochastic processes in solar flares.
学科主题Astronomy & Astrophysics
WOS标题词Science & Technology ; Physical Sciences
类目[WOS]Astronomy & Astrophysics
研究领域[WOS]Astronomy & Astrophysics
关键词[WOS]PERIOD NETWORK OSCILLATIONS ; SOLAR-FLARE ; EXPLOSIVE EVENTS ; MAGNETIC RECONNECTION ; TRANSITION REGION ; ELECTRON-BEAMS ; ACCELERATION ; WAVES ; JETS ; SUN
收录类别SCI
语种英语
WOS记录号WOS:000229978400031
公开日期2012-03-07
内容类型期刊论文
源URL[http://159.226.72.40/handle/332002/4090]  
专题紫金山天文台_南极天文中心
作者单位1.Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China
2.Purple Mt Observ, Nanjing 210093, Peoples R China
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GB/T 7714
Ning, Z,Ding, MD,Wu, HA,et al. Microwave type III bursts and pulsation groups[J]. ASTRONOMY & ASTROPHYSICS,2005,437(2):691-697.
APA Ning, Z,Ding, MD,Wu, HA,Xu, FY,&Meng, X.(2005).Microwave type III bursts and pulsation groups.ASTRONOMY & ASTROPHYSICS,437(2),691-697.
MLA Ning, Z,et al."Microwave type III bursts and pulsation groups".ASTRONOMY & ASTROPHYSICS 437.2(2005):691-697.
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