Abstract
Problems of “weak” magnetic fields diagnostics in the upper solar atmosphere are discussed, where the Zeeman splitting is 3-4 orders of magnitude less than the line width. This corresponds to magnetic observations of chromosphere, prominences and the corona requiring more advanced technique as compared with the photosphere. Direct and indirect methods of magnetic researches in the upper solar atmosphere are briefly reviewed. The “signal-to-noise” ratio of magnetic records is shown to strongly depend on the stray light in the feeding telescope. Concordance of performances of a feeding telescope and Stokes polarimeter are analysed to carry out reliable magnetic measurements. Eclipse coronagraphic polarimetric observations are concluded to be powerful for low-resolution magnetic diagnostics based on analysis of Hanle effect in prominences and the emission line corona. Employment of a new generation large-aperture reflecting coronagraph allows to expect advances in high-resolution magnetic observations of prominence and coronal structures.
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Kim, I.S. (2000). Observing the Solar Magnetic Field. In: Zahn, JP., Stavinschi, M. (eds) Advances in Solar Research at Eclipses from Ground and from Space. NATO Science Series, vol 558. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4325-7_5
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DOI: https://doi.org/10.1007/978-94-011-4325-7_5
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