用SOLARC测量太阳日冕磁场
The Solar Coronal Magnetic Field Measurements With SOLARC
摘要：
由于最近发展了高灵敏度红外探测技术，直接测量太阳日冕磁场已成为可能。安装在Mt. Haleakala就是这样一个偏振日冕仪，它被设计用于常规观测近红外（NIR）波段的斯托克斯参数分布。Fe $^{+12}$ 1075 nm禁戒日冕发射线（CEL）具有探测弱日冕磁场的潜力。作为第一步，势场模型已被用于与Fe $^{+12}$ 1075 nm谱线中的SOLARC观测结果进行比较（Liu和Lin，2008年）。结果表明，位场可以作为一个零级代用指标，用来逼近简单稳定黑子上方观测到的日冕场。在本文中，我们进一步讨论了几个阻碍重建真实日冕磁场结构的节点。它们包括线性偏振信号中众所周知的Van Vleck效应，对NIR发射源的信息的忽略（即，日冕磁场的反演问题），大量的全球非线性无力场工具可用于更好地模拟日冕磁场，等等。
英文摘要：
Direct solar coronal magnetic field measurements have become possible since recent development of high-sensitivity infrared detection technology. The SOLARC instrument installed on Mt. Haleakala is such a polarimetric coronagraph that was designed for routinely observing Stokes parameter profiles in near infrared (NIR) wavelengthes. The Fe$^{+12}$ 1075 nm forbidden coronal emission line (CEL) is potential for weak coronal magnetic field detection. As a first step the potential field model has been used to compare with the SOLARC observation in the Fe$^{+12}$ 1075 nm line (Liu and Lin 2008). It's found that the potential fields can be a zeroth-order proxy for approaching the observed coronal field above a simple stable sunspot. In this paper we further discuss several nodi that are hampering the progress for reconstructing the real coronal magnetic field structures. They include the well-known Van Vleck effect in linear polarization signals, ignorance of the information of the NIR emission sources (i.e., inversion problem of coronal magnetic fields), a fat lot of global non-linear force-free field tools available for better modeling coronal magnetic fields, and so on.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
