YNAO OpenIR  > 太阳物理研究组
Alternative TitleThe relations between the magnetic properties and the geometrical properties
Thesis Advisor屈中权
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太阳黑子 磁场 反演方法 黑子几何特性
Abstract黑子是太阳表面磁场最密集的地方,每个发育完整的黑子都是由本影、半影组成。我们对太阳黑子特征突破性的理解是在1908年,当时George Ellery Hale第一次测量了黑子的磁场,从那时起磁场作为黑子形成的最主要原因就建立了起来。由于黑子的磁场无法直接测得,因此目前主要是利用太阳斯托克斯参量测量得出黑子磁场信息。人们经常根据大气模型重构出观测的谱线轮廓,然后把拟合轮廓和观测轮廓进行对比,如果不满足拟合的条件就改变模型,直到达到满意的拟合效果。最近在得出黑子磁场信息的方法中,反演方法越来越盛行。反演方法一般根据最小二乘法找到一个最小的量(观测轮廓和拟合轮廓的平方差),而由最小二乘反演出的物理参量反映了太阳活动区大气的特征。 本篇论文的结构如下:在第一章简单介绍了黑子可观测的基本知识;第二章主要介绍偏振辐射转移方程,方程的解,以及利用偏振辐射转移反演得出磁场信息的几种方法;第三章介绍了作者利用反演方法得出磁场信息,从而分析黑子的磁场特性与几何特性的关系。 本文侧重于黑子的几何特征与磁场特性的关系。作者通过统计研究发现:黑子的最大磁场与黑子面积,本影面积的关系都呈现对数的形式;而无论是黑子最大磁场还是纵向磁场都随着半影-本影半径比率的增加而逐渐减小。因此,在模拟黑子的时候,半影-本影的半径比率、黑子面积、本影面积都变成重要的参量。
Other AbstractSunspots are the most visible manifestations of solar magnetic field concentration. Each well developed sunspot is characterized by the umbra and penumbra.The breakthrough in our understanding of the nature of sunspots came in 1908 when George Ellery Hale first measured a magnetic field in sunspots. Since then the magnetic field has become firmly established as the root cause of the sunspot phenomenon. Because the magnetic field cannot be directly observed, adopting spectrum analysis to obtain magnetic field has become the major technique recently. More frequently, an initial guess of model atmosphere is constructed and used to calculate line profiles. These are then compared with observations. If correspondence between synthetic and observed profiles is insufficient, the model is changed. This process is repeated until a satisfactory fit is achieved. Recently, so-called inversion techniques have become more popular. In general, the least-square fit technique is employed to find a minimum (squared difference between observed and synthetic Stokes parameters). The inversed physical parameters by the minimization, therefore, reflect the atmosphere characters of active region. This thesis simply introduces the sunspot basic knowledge observed in chapter 1. Polarised radiation transfer equations, the solution of it and some inversion techniques making use of radiation transfer equations are recommended in chapter 2. The author adopts inversion technique to obtain magnetic field and analyzes the relation between the magnetic properties of sunspots and their geometrical properties in chapter 3. The thesis is to pay more attention to the relation between the magnetic properties of sunspots and their geometrical properties. The authors find by statistically researching:the relations of the maximum magnetic field with sunspot area and umbral area are the logarithmic expressions; whether maximum magnetic field or longitudinal magnetic field decrease with increasing penumbra-umbra radius ratio. Therefore, in simulating sunspots, the penumbra-umbra radius ratio, umbral area and penumbral area become significant parameters.
Subject Area天文学
Document Type学位论文
Recommended Citation
GB/T 7714
金春兰. 黑子的磁场性质与几何性质之间的关系[D]. 北京. 中国科学院研究生院(云南天文台),2006.
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