.png){kind=icon}
返回
Magnetohydrodynamic Waves in Open Coronal Structures
.png){kind=icon}
PRE
AI
DOI：10.1007/s11214-021-00849-0.png)
.png){kind=icon}
原文求助.png){kind=icon}
分享.png){kind=icon}
收藏
摘要
En 中文
Modern observatories have revealed the ubiquitous presence of magnetohydrodynamic waves in the solar corona. The propagating waves (in contrast to the standing waves) are usually originated in the lower solar atmosphere which makes them particularly relevant to coronal heating. Furthermore, open coronal structures are believed to be the source regions of solar wind, therefore, the detection of MHD waves in these structures is also pertinent to the acceleration of solar wind. Besides, the advanced capabilities of the current generation telescopes have allowed us to extract important coronal properties through MHD seismology. The recent progress made in the detection, origin, and damping of both propagating slow magnetoacoustic waves and kink (Alfvenic) waves is presented in this review article especially in the context of open coronal structures. Where appropriate, we give an overview on associated theoretical modelling studies. A few of the important seismological applications of these waves are discussed. The possible role of Alfvenic waves in the acceleration of solar wind is also touched upon.
Keyword:
Solar corona
Magnetohydrodynamics
Waves and oscillations
期刊
IF:
7.4
论文数:
4.2K
被引数:
1.8W
机构
引用论文
Generalized phase mixing: Turbulence-like behaviour from unidirectionally propagating MHD waves.png)
SCIENTIFIC REPORTS
OAAI
SCIENTIFIC REPORTSIF3.9
OAAI分享收藏FORWARD MODELING OF PROPAGATING SLOW WAVES IN CORONAL LOOPS AND THEIR FREQUENCY-DEPENDENT DAMPINGOAAI
OAAI分享收藏分享收藏OBSERVATIONAL QUANTIFICATION OF THE ENERGY DISSIPATED BY ALFVEN WAVES IN A POLAR CORONAL HOLE: EVIDENCE THAT WAVES DRIVE THE FAST SOLAR WIND极地日冕洞中ALFVEN波耗散的能量的观测量化: 波驱动快速太阳风的证据OAAI
OAAI分享收藏
查看更多内容