YNAO OpenIR  > 太阳物理研究组
太阳活动区观测研究
其他题名Observations Study of Solar Active Region
李珂君
学位类型硕士
导师姜云春
2009
学位授予单位中国科学院研究生院(云南天文台)
学位授予地点北京
学位专业天体物理
关键词太阳 - 活动区 太阳 - 磁场 太阳 - 黑子 太阳 - 光球 太阳 - 色球
摘要太阳是离地球最近的恒星,与人类的生产生活息息相关,太阳所散发的光、 热为地球保持了生命存在和发展提供了必要条件。然后太阳活动及周期性的变 化,对人类的生存环境有着直接影响,这些影响有的是对人类有益的,但是很多 却是不利的。而太阳的活动多数来自于太阳上的活动区,对此我们有必要研究 太阳活动区的各种物理现象探索其物理本质。 本文是一篇运用高分辨率空间望远镜对太阳活动区的观测进行研究论文。 本文分为一下几个部分: 第一章:太阳活动区的基本知识和概述:包括活动区的形成与消亡,黑子 的基本知识,以及活动区内的小尺度结构的介绍。 第二章:我们运用Hinode 和STEREO 的G-band、Ca ii-H、磁图、软X 射 线和171 ºA的单色像对2007 年3 月8 日出现在日面中心的一个新浮磁流区进行 观测研究。通过对该新浮磁流区演化的观测,我们发现新浮磁流区的两极转动 违反Joy's 定律,各个太阳大气光变曲线的测量及冕环收缩两方面的研究为活 动区上方冕环形成主要是从热环冷却成为冷环的冕环形成机制提供证据支持, 并且证实新浮磁流区上方的冕环在演化过程中产生收缩冷却。这为太阳活动周 期磁场的变化研究、活动区上方日冕加热与收缩冷却的机制提供了重要的观测 数据,为将来相关方面数值模拟的研究提供很好的观测证据。 第三章:我们运用Hinode 的G-band、Ca ii-H 和磁图对出现在两个衰减活 动区内的偶极运动磁特征进行观测研究,发现:偶极运动磁特征出现在黑子半 影内部,主要与半影暗纤维和Evershed 流相关,这说明偶极运动磁特征在向外 运动的同时将Evershed 物质沿着水平磁场带到黑子外。另外,偶极运动磁特征 出现后光球层和色球层有点状增亮响应。上述两点可能说明:首先运动磁特征 与黑子或者活动区的衰减有关,第二偶极运动磁特征引起的低色球增亮响应可 能是黑子半影的低色球层以下的一种加热机制。 第四章:对全文进行总结和未来工作的展望。
其他摘要The Sun is the nearest star to the earth, and be connected to the working and living of human. Because of the light and heat of sun giving, the beings can exist on the earth. Moreover, the solar activities and periodic changes of the sun could a®ect the living environment the human beings. Not every activities is good for human. And most of those activities are original from the Active Region (AR), So we must research diversity activities of AR and explore the physical essence. The thesis is dedicated to the research the observations of solar AR with high resolution Telescope. It is structured as follow: In chapter one, on the base of surveying a number of references, we sum- marized the basic knowledge to the formation and decaying of AR, sunspots and small scaled structures of AR. In chapter two, we have investigated the formation and high atmosphere response of an emerging °ux region (EFR) near the solar disk center on equator with Hinode and STEREO. By analysing those, we derived the following results: (1) The rotation of bipolar polarity of the EFR was against Joy's law. (2)By measure the variation of inversion line of the EFR, seperation speed of the bipolar polarity and rotation angle with equator, the EFR was highly twisted magnetic °ux ¯eld. (3)There were dark lanes connected new emerging °ux tubes, which was accompanied by two light points near the end of dark lane. These dark lanes could last about 10min. (4)High atmosphere response light curve display: chromosphere Caii-H ¯rst response the EFR, second was soft X-Ray, the last was 171 ºA. These means the formation of warm coronal loop was trigged by cooling the hot coronal loop. (5) By measure the area of EFR in soft X-Ray images, the coronal loops may shrink, this also support the idea of (4). In chapter three, we have investigated 35 obvious bipolar moving magnetic features (MMFs) with Hinode ¯ltergrams and magnetograms, which appear in sunspot penumbra. From analysis their change of the con¯guration, speed and the lightening response of the low solar atmosphere, we derived the following results: (1) Bipolar MMFs appear in middle penumbra, and they occur between penumbral ¯laments with enhanced longitudinal magnetic signals. Both polarity of bipole move radially outward. This indirect supports the idea that the origin of the bipolar MMFs is on the horizontal magnetic ¯eld of the penumbra. There are more than one pair of bipolar MMFs appearing at the same position in 2 hour-8 hour. And this provides the evidence of sea-serpent ¯eld lines model. (2) The lightening response in photosphere and chromospheres illuminates that the motion of the bipoles could heat the low solar atmosphere. (3) The position of bipolar magnetic structures and magnetic ¯eld distribution of sunspot penumbra add another piece of evidence in favor of the uncombed structure of penumbral magnetic ¯elds. In chapter four, we describe the conclusion from the above studies and the future of our work.
学科领域天文学
页数73
语种中文
文献类型学位论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/6604
专题太阳物理研究组
推荐引用方式
GB/T 7714
李珂君. 太阳活动区观测研究[D]. 北京. 中国科学院研究生院(云南天文台),2009.
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