日冕中EUV波的研究进展
Progress of the Study on the Coronal EUV Waves
查看参考文献93篇
|
文摘
|
日冕极紫外(EUV)波是Thompson等人1998年首先在EIT的观测资料中发现的,在日冕中以几百km/s 的速度传播的扰动现象,在1 h之内扫过了大部分太阳表面,所以这个现象开始被称为“EIT 波”。首先介绍了EUV波的研究背景;然后介绍了EUV波的观测特征;第3章分别介绍了EUV波与Moreton波、耀斑及CME 的关系;第4章介绍了从发现EUV波以来提出的各种理论和模型;第5章讨论到目前为止已发现的EUV波成分:一个较快的波在前面传播,一个较慢的波在后面传播;最后,对EUV波研究的未来方向及发展趋势进行了总结和展望。 |
|
其他语种文摘
|
Extreme Ultraviolet (EUV) waves are large-scale disturbances in the corona. They can pass through the whole solar disk in an hour at the speed of hundreds of kilometers per second. The EUV wave was first discovered by Thompson (1998) when the data from the EUV Imaging Telescope (EIT) were studied. So it was originally named EIT wave. It is now generally called EUV wave since its appearance and properties are not dependent on a specific instrument, and ‘EUV’ is more appropriate for describing one of its important physical features. The EUV wave usually has a bright broad relatively-diffuse circular wavefront followed by an expanding dimming region. The EUV wave is thought to be the counterpart of the chromospheric Moreton wave in the corona. However, very few observation including both phenomena has been reported. Moreover, observations showed that EUV waves have two components, a faster wave in front and a slower wave following. These all indicate that the EUV wave and the Moreton wave are not the same. Though having been studied for years, the physical nature and the driving mechanism of EUV waves still remain unclear. Solar flares and coronal mass ejections(CMEs) are the two candidates to drive EUV waves. Currently, both theoretical and observational studies suggested that the flare cannot cause EUV wave, while CME is more likely to drive the EUV wave. In addition, whether EUV waves are the wave or the pseudo-wave or the hybrid wave is still unknown. There are five possible mechanisms for explaining EUV waves: fast mode MHD waves, magnetic field lines successively stretching, successive reconnection, current shell, and slow mode wave or solitary wave. The prevailing scenario of explaining the observational charac-teristics of EUV waves is of the combination of the first two. Take advantage of the high resolution telescope, we are convinced that EUV waves possess two components, which is supported by many observational evidences. However there are still many unsolved problems, and we hope that we can solve them in the future by development of the numerical simulations and observations of high spatial resolution and high time cadence. |
|
来源
|
天文学进展
,2014,32(3):259-281 【核心库】
|
|
关键词
|
EUV波
;
Moreton波
;
日冕物质抛射
;
耀斑
;
快模磁流体动力学波
;
慢模磁流体动力学波
|
|
地址
|
1.
中国科学院云南天文台, 云南, 昆明, 650011
2.
云南大学物理科学技术学院, 云南, 昆明, 650031
3.
云南师范大学旅游地理学院, 云南, 昆明, 650031
|
|
语种
|
中文 |
|
文献类型
|
综述型 |
|
ISSN
|
1000-8349 |
|
学科
|
天文学 |
|
基金
|
国家973计划
;
国家自然科学基金
;
中国科学院知识创新工程重要方向项目
|
|
文献收藏号
|
CSCD:5232975
|
参考文献 共
93
共5页
|
|
1.
Delaboudiniμere J P.
Sol. Phys,1995,162:291
|
被引
1
次
|
|
|
|
|
2.
Thompson B J.
Geophys. Res. Lett,1998,2465:2468
|
被引
1
次
|
|
|
|
|
3.
Thompson B J.
ApJ,1999,517:L151
|
被引
14
次
|
|
|
|
|
4.
Biesecker D A.
ApJ,2002,569:1009
|
被引
11
次
|
|
|
|
|
5.
Wuelser J P.
Proc. SPIE., 5171,2004:111
|
被引
1
次
|
|
|
|
|
6.
Lemen J R.
Sol. Phys,2011,275:17
|
被引
2
次
|
|
|
|
|
7.
Athay R G.
ApJ,1961,133:935
|
被引
2
次
|
|
|
|
|
8.
Uchida Y.
Sol. Phys,1968,4:30
|
被引
9
次
|
|
|
|
|
9.
Warmuth A.
ApJ,2001,560:L105
|
被引
6
次
|
|
|
|
|
10.
Warmuth A.
A&A,2004,418:1101
|
被引
4
次
|
|
|
|
|
11.
Warmuth A.
A&A,2004,418:1117
|
被引
4
次
|
|
|
|
|
12.
Chen P F.
ApJ,2005,622:1202
|
被引
11
次
|
|
|
|
|
13.
Chen P F.
ApJ,2002,572:L99
|
被引
22
次
|
|
|
|
|
14.
Eto S.
PASJ,2002,54:481
|
被引
5
次
|
|
|
|
|
15.
林元章.
太阳物理导论,2000:527
|
被引
2
次
|
|
|
|
|
16.
Priest E R.
The Astron Astrophys Rev,2002,10:313
|
被引
30
次
|
|
|
|
|
17.
Chen P F.
ApJ,2006,641:L153
|
被引
10
次
|
|
|
|
|
18.
林元章.
太阳物理导论,2000:460
|
被引
2
次
|
|
|
|
|
19.
Gopalswamy N.
20th National Solar Physics Meeting. 1,2010:108
|
被引
1
次
|
|
|
|
|
20.
Chen P F.
Living Rev. Sol. Phys,2011,1:92
|
被引
1
次
|
|
|
|
|
了解气象卫星更多信息，请访问