Localized Microwave and EUV Bright Structures in an Eruptive Prominence

doi:10.3847/1538-4357/ab0e80

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	Localized Microwave and EUV Bright Structures in an Eruptive Prominence
	Huang,Jing 4; Tan,Baolin 4; Masuda,Satoshi 3; Cheng,Xin 2; Kumar Bisoi,Susanta 4; Melnikov,Victor 1,4
刊名	The Astrophysical Journal
	2019-04-05
卷号	874 期号:2
关键词	Sun: filaments, prominences Sun: particle emission Sun: radio radiation Sun: UV radiation
ISSN号	0004-637X
DOI	10.3847/1538-4357/ab0e80
英文摘要	Abstract We study a solar eruptive prominence with flare/coronal mass ejection (CME) event by microwave and extreme ultraviolet (EUV) observations. Its evolution can be divided into three phases: slow rise, fast expansion, and ejection. In the slow-rise phase, the prominence continuously twists for more than one hour with a patch of bright emission appearing around the top. When the north leg interacts with the local small-size loops, the fast expansion is initiated and the flare takes place there. The prominence grows rapidly, and a series of localized brightenings appear in the whole prominence structure. Then the ejection occurs, followed by a CME. In microwave images, the brightness temperature (Tb) at 17 and 34 GHz can be divided into three components. The strongest emission with Tb at 25,000–300,000 K is related to the bright flare region near the north foot. The medium Tb (10,000–20,000 K) outlines a series of small-scale bright enhancements scattering in the prominence, which are superposed on a weak background with Tb at 5000–10,000 K. These localized bright structures, first appearing at the top and then scattering in the entire prominence structure, are cospatial with EUV bright threads, fibers, or spots in both high- and low-temperature passbands. They display significant temporal variations on the scale of 3–5 s in the microwave observations. Thus, the plasma inside the prominence is spatially structured and changes with time in both density and temperature. This behavior could be interpreted in the frame of the small-scale and short-term process of energy releases in the twisted magnetic structure.
语种	英语
出版者	The American Astronomical Society
WOS记录号	IOP:0004-637X-874-2-AB0E80
内容类型	期刊论文
源URL	[http://ir.bao.ac.cn/handle/114a11/28808]
专题	中国科学院国家天文台
作者单位	1.Central (Pulkovo) Astronomical Observatory, Russian Academy of Sciences, St. Petersburg, Russia 2.School of Astronomy and Space Science, Nanjing University, Nanjing 210093, People’s Republic of China 3.Institute for Space and Earth Environmental Research, Nagoya University, Nagoya 464-8601, Japan 4.CAS Key Laboratory of Solar Activities, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People’s Republic of China; huangj@bao.ac.cn
推荐引用方式 GB/T 7714	Huang,Jing,Tan,Baolin,Masuda,Satoshi,et al. Localized Microwave and EUV Bright Structures in an Eruptive Prominence[J]. The Astrophysical Journal,2019,874(2).
APA	Huang,Jing,Tan,Baolin,Masuda,Satoshi,Cheng,Xin,Kumar Bisoi,Susanta,&Melnikov,Victor.(2019).Localized Microwave and EUV Bright Structures in an Eruptive Prominence.The Astrophysical Journal,874(2).
MLA	Huang,Jing,et al."Localized Microwave and EUV Bright Structures in an Eruptive Prominence".The Astrophysical Journal 874.2(2019).