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Direct solar coronal magnetic field measurements have become possible sincerecent development of high-sensitivity infrared detection technology. TheSOLARC instrument installed on Mt. Haleakala is such a polarimetric coronagraphthat was designed for routinely observing Stokes parameter profiles in nearinfrared (NIR) wavelengthes. The Fe$^{+12}$ 1075 nm forbidden coronal emissionline (CEL) is potential for weak coronal magnetic field detection. As a firststep the potential field model has been used to compare with the SOLARCobservation in the Fe$^{+12}$ 1075 nm line (Liu and Lin 2008). It's found thatthe potential fields can be a zeroth-order proxy for approaching the observedcoronal field above a simple stable sunspot. In this paper we further discussseveral nodi that are hampering the progress for reconstructing the realcoronal magnetic field structures. They include the well-known Van Vleck effectin linear polarization signals, ignorance of the information of the NIRemission sources (i.e., inversion problem of coronal magnetic fields), a fatlot of global non-linear force-free field tools available for better modelingcoronal magnetic fields, and so on.

The Solar Coronal Magnetic Field Measurements With SOLARC