Abstract
After having presented the magnetic field effects on the radiation emitted in an atomic or molecular line (Zeeman effect, Hanle effect), we present two applications: (i) the measurement of the magnetic field vector in solar prominences during the ascending phase of Cycle XXI. By transferring the results on synoptic maps of the filaments, a general organization of the large-scale surface field becomes visible; (ii) the measurements of the surface magnetic field made by recent spectropolarimeters like THEMIS. The result is the division of the surface magnetic field into two classes: (a) the network field, nearly vertical and 100 G or more (local average value), located in active regions and at the frontiers of supergranules; (b) the internetwork field, turbulent in direction with an horizontal trend, with a local average value of 20 Gauss or less.
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Bommier, V. (2009). The Solar Magnetic Field: Surface and Upper Layers, Network and Internetwork Field. In: Rozelot, JP., Neiner, C. (eds) The Rotation of Sun and Stars. Lecture Notes in Physics, vol 765. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-87831-5_10
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DOI: https://doi.org/10.1007/978-3-540-87831-5_10
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