The Solar Coronal Magnetic Field Measurements With SOLARC

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dc.creatorLiu, Y.
dc.creatorLin, H.
dc.date2008-09-04
dc.date2008-09-05
dc.date.accessioned2026-07-07T10:00:37Z
dc.date.available2026-07-07T10:00:37Z
dc.descriptionDirect 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.
dc.description3 pages, 4 figs, APRIM 2008 Proceedinds
dc.identifierhttps://arxiv.org/abs/0809.0729
dc.identifierhttp://arxiv.org/abs/0809.0729
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/168371
dc.subjectAstrophysics
dc.titleThe Solar Coronal Magnetic Field Measurements With SOLARC
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