The Solar Coronal Magnetic Field Measurements with SOLARC
Direct solar coronal magnetic field measurements have become possible since recent development of high-sensitivity infrared detection technology. The SO LARC 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 8tep the potential field model has been used to compare with the SOLARC observation in the Fe+12 1075 nm line (Liu & Lin 2008). Its found that the potential fields can be & zeroth-order proxy for approaching the observed coronal field above a simple 8table sunspot. In this paper we further discuss several nodi that are hampering the progress for reconstructing the real coronal magnetic field 8tructures. They include the well-known Van Vleck effect in lin ear 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.
Sun corona Sun magnetic field
Y.Liu H.Lin
Yunnan Astronomical Observatory / National Astronomical Observatories, Kunrning,China Institute for Institute for Astronomy,University of Hawaii,Hawaii,USA
国际会议
The 10th Asian-Pacific Regional International Astronomical Union Meeting(第十届亚洲及太平洋地区天文学大会 APRIM)
昆明
英文
53-56
2008-08-03（万方平台首次上网日期，不代表论文的发表时间）