High Spatial Resolution Solar Microwave Observations
High Spatial Resolution Solar Microwave Observations
复制标题
高空间分辨率太阳微波观测
DOI：
10.1146/annurev.aa.20.090182.002433
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发表时间：
1982
影响因子：
33.3
通讯作者：
G. Hurford
中科院分区：
文献类型：
--
作者：
G. Hurford
讨论了高光谱分辨率微波观测在研究太阳活动方面的应用，特别强调了太阳活动区微波辐射的频率依赖性。一个壳模型的陀螺共振发射活动区的说明，这表明，高光谱分辨率，空间分辨观测可以提供定量信息的磁场分布在该基地的日冕。本文给出了用欧文斯谷捷频干涉仪在1.2 ~ 14 Ghs的56个频率上对单个太阳黑子的相应观测结果。尽管存在潜在物理意义上的差异，但观察到的尺寸和亮温谱的总体形式与基于壳模型的预期一致。简要讨论了微波光谱学作为日冕磁场测量技术的优点和缺点。
The application of high-spectral resolution microwave observations to the study of solar activity is discussed with particular emphasis on the frequency dependence of microwave emission from solar active regions. A shell model of gyroresonance emission from active regions is described which suggest that high-spectral resolution, spatially-resolved observations can provide quantitative information about the magnetic field distribution at the base of the corona. Corresponding observations of a single sunspot with the Owens Valley frequency-agile interferometer at 56 frequencies between 1.2 and 14 Ghs are presented. The overall form of the observed size and brightness temperature spectra was consistent with expectations based on the shell model, although there were differences of potential physical significance. The merits and weaknesses of microwave spectroscopy as a technique for measuring magnetic fields in the solar corona are briefly discussed.