YNAO OpenIR  > 选址与日冕观测组
Alternative TitleStudy of the morphology and fluctuation of solar spicules
Thesis Advisor刘煜
Degree Grantor中国科学院研究生院(云南天文台)
Place of Conferral北京
Degree Discipline天体物理
Keyword针状体 磁重联 纤维 日芒
Abstract色球层是太阳大气层中一个很重要的层次,位于光球和过渡区及日冕层之间,色球层的厚度约为1500公里。通过色球谱线(如H-alpha, Ca ii的H线或K线)可以看到太阳色球层有很多重要结构和爆发现象:针状体、谱斑、网络结构、暗条、日芒、纤维、快速蓝移事件等。得益于SST、SOT/Hinode等高分辨太阳望远镜的投入使用,针状体及日芒、纤维的研究有了很大突破。本论文详细调研和总结了国内外围绕太阳针状体研究的高分辨观测成果以及相关理论研究进展,主要分为以下几个部分: 第一章主要介绍了针状体的形态和分类以及在其它区域和谱线观测到的针状体对应物。 第二章介绍了针状体的震荡以及引起这些震荡的波动。针状体在向上传播的过程中,能够观测到垂直于针状体传播方向的摆动,这种摆动称为横向震荡,很可能是由阿尔芬波或者扭结波引起的。 第三章介绍了引发针状体针状体的各种机制,重点介绍了激波激发机制和磁重联机制。 第四章,我们对SOT/Hinode观测的一部分针状体做形态与波动的分析。背景会对针状体的寿命造成一定的影响,我们认为对于受背景影响严重的针状体应该利用外推法来测得寿命;针状体的震荡可能会影响到针状体分类的判断;我们观测到了一例阻尼随高度减小的针状体。借助于云南天文台一米红外望远镜NVST,我们未来的工作主要包括两个部分:(1)更加深入的探究针状体的震荡对针状体分类的影响;(2)针状体这种阻尼减少和物质密度的关系。最后对对本论文进行总结和展望
Other AbstractThe chromosphere, one of the most important atmosphere of the sun, is sandwiched between the photosphere and the transition region and the corona. Its thickness is about 1500km. Lots of significant structures and eruptions can be seen in chromospheric spectral lines (H-alpha, Ca ii H or K), such as spicules, plages, networks, filaments, mottles, fibrils, RBEs (Rapid Blueshift Events) and so on. Owing to the use of the solar high resolution telescopes (SST and SOT/Hinode) there are great breakthroughs on the research about spicules, mottles and fibrils. In this thesis we focus on the high resolution observations and related theoretical research of spicules. The structure of the thesis is as follows: In chapter one, we introduce the morphology and classification of spicules. The counterparts of spicules in other regions and lines are also discussed. In chapter two, we introduce the oscillation and related fluctuation of spicules. Spicules undergo transverse oscillation, i.e., oscillation that appears to be transverse to the spicule long axis when they propagate upward. The oscillation period is about 100-500s and the velocity is about 10-25km/s. The oscillation may be motivated by alfv′en or kink wave. In chapter three, we introduce the driving mechanisms of spicules, and we focus on the shock and magnetic reconnection mechanisms. In chapter four, we study the morphology and fluctuation of spicules observed by SOT on-board Hinode. We think we should use extrapolation method to estimate the lifetime of spicules which is influenced seriously by background. The oscillation may affect the classification of spicules. We find oscillation damping decrease with height. By using the NVST (the New Vacuum Solar Telescope) in Yunnan Observatories, the future work contains two sections: (1) how oscillation affects classification; (2) the relationship between damping decrease and mass density. Finally, it is the study conclusion and adaptation prospect.
Subject Area天文学
Document Type学位论文
Recommended Citation
GB/T 7714
赵瑞娟. 太阳针状体的形态与波动分析[D]. 北京. 中国科学院研究生院(云南天文台),2014.
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