The Fe XIII 10747 and 10798 ? lines observed in the solar corona are sensitive to the coronal magnetic field in such a way that, in principle, the full vector field at a point on the line of sight can be inferred from their combined polarization signals. This paper presents analytical inversion formulae for the field parameters and analyzes the uncertainty of magnetic field measurements made from such observations, assuming emission dominated by a single region along the line of sight. We consider the case of the current Coronal Multi-channel Polarimeter (CoMP) instrument as well as the future Coronal Solar Magnetism Observatory (COSMO) and Advanced Technology Solar Telescope (ATST) instruments. Uncertainties are estimated with a direct analytic inverse and with a Markov Chain Monte Carlo algorithm. We find that (in effect) two components of the vector field can be recovered with CoMP, and well recovered with COSMO or ATST, but that the third component can only be recovered when the solar magnetic field is strong and optimally oriented.
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机译：Fe XIII 10747和10798？在日冕中观察到的直线对日冕磁场敏感，因此，原则上可以从它们的组合极化信号中推断出视线上某个点的全矢量场。本文介绍了场参数的解析反演公式，并分析了由这些观测值得出的磁场测量值的不确定性，并假设辐射由沿视线的单个区域主导。我们考虑了当前的日冕多通道旋光仪（CoMP）以及未来的日冕太阳磁观测站（COSMO）和先进技术太阳望远镜（ATST）仪器的情况。用直接解析逆和马尔可夫链蒙特卡罗算法估计不确定性。我们发现（实际上）向量场的两个分量可以使用CoMP进行恢复，并且可以使用COSMO或ATST很好地进行恢复，但是只有在太阳磁场强且方向最优时，才能恢复第三分量。
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