• ISSN 2097-1893
  • CN 10-1855/P
引用本文: 杨子浩,田晖,李文显,张佳乐,白先勇,高宇航,陈亚杰. 2022. 日冕磁场测量. 地球与行星物理论评,53(4):379-396
Yang Z H, Tian H, Li W X, Zhang J L, Bai X Y, Gao Y H, Chen Y J. 2022. Research progress in coronal magnetic field measurements. Reviews of Geophysics and Planetary Physics, 53(4): 379-396

日冕磁场测量

doi: 10.19975/j.dqyxx.2022-010
基金项目: 国家重点研发计划资助项目(2021YFA0718600)
详细信息
    作者简介:

    杨子浩(1996-),男,博士研究生,主要从事日冕磁场测量和日冕光谱诊断方面的研究. E-mail:yangzihao96@pku.edu.cn

    通讯作者:

    田晖(1982-),男,教授,主要从事太阳活动与空间天气的研究. E-mail:huitian@pku.edu.cn

    李文显(1989-),女,研究员,主要从事太阳物理、原子结构计算方面的研究. E-mail:wxli@nao.cas.cn

  • 中图分类号: P182

Research progress in coronal magnetic field measurements

Funds: Supported by the National Key R&D Program of China(Grant No. 2021YFA0718600)
  • 摘要: 磁场把太阳的各层大气耦合在一起,并主导着其中的各种物理过程,磁场的演化引发包括太阳爆发在内的活动现象,进而影响着地球的空间环境和人类的生存条件. 要理解发生在太阳大气中的各种活动现象,离不开对其磁场的完整认知. 然而目前对太阳高层大气尤其是日冕的磁场测量仍然严重缺失,这大大限制了人类对太阳活动的研究,制约了太阳物理和空间天气学科的发展. 经过几十年的探索,人们提出了几种可能可用于日冕磁场诊断的方法,包括利用日冕红外谱线的偏振观测、借助射电波段的日冕辐射、通过日冕中各类波动的冕震学诊断以及利用日冕极紫外谱线的磁场诱导跃迁原理对日冕磁场进行测量等. 同时,人们也根据这些方法尝试对日冕磁场进行了测量,取得了一些进展. 本文总结了几种主要的日冕磁场测量方法的原理和重要进展,并对未来的相关研究做了展望.

     

  • 图  1  塞曼效应的经典描述图像. 从不同方向观测到的偏振特性不同,分别对应着纵向塞曼效应和横向塞曼效应(修改自Lites, 2000

    Figure  1.  The classical description of longitudinal and transverse Zeeman effect. The observed polarization states vary with the observer's viewing direction (modified from Lites, 2000)

    图  2  观测到的Fe XIII 10747 Å的斯托克斯QV轮廓,可以看到斯托克斯V的反对称轮廓(修改自Lin et al., 2000

    Figure  2.  The observed profiles of Stokes Q and V from Fe XIII 10747 Å, the anti-symmetric profile of Stokes V was clearly observed (modified from Lin et al., 2000)

    图  3  使用EOVSA观测到的回旋同步加速辐射诊断得到的耀斑区域的二维日冕磁场分布的时间演化. (a)~(d)代表不同的时刻(修改自Fleishman et al., 2020

    Figure  3.  Temporal evolution of coronal magnetograms in a flare region, as diagnosed through gyrosynchrotron emissions observed with EOVSA (modified from Fleishman et al., 2020)

    图  4  对CoMP观测到的扭曲模行波做冕震学诊断得到的日冕磁场的全局性分布图(修改自Yang et al., 2020a

    Figure  4.  Global map of coronal magnetic field obtained through magnetoseismology using CoMP observations (modified from Yang et al., 2020a)

    图  5  利用前向模拟验证磁场诱导跃迁方法可行性的结果. (a,c)模型中日面上和日轮边缘外(视线方向垂直日面和平行日面)的日冕磁场强度分布. (b,d)根据前向模拟,利用MIT方法诊断得到的磁场强度(修改自Chen et al., 2021

    Figure  5.  (a, c) Spatial distributions of coronal magnetic field strength in the model for disk-center and off-limb views, respectively. (b, d) The derived magnetic field strength based on the MIT technique using forward modelling (modified from Chen et al., 2021)

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出版历程
  • 收稿日期:  2022-01-29
  • 录用日期:  2022-03-05
  • 网络出版日期:  2022-03-28
  • 刊出日期:  2022-05-11

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