Abstract
The three-dimensional shape of coronal magnetic loops is restored from extreme ultraviolet (XUV) images of the Sun (Skylab mission 3, 1973) by using the perspective effect due to the solar rotation. An original method is developed which only depends on the assumption that the magnetic structures under consideration are (at least geometrically) stable within the time interval used for restoration. Large scale loops interconnecting different active regions are studied by applying this method. They are found to lie approximately in planes inclined from the local vertical. Generally these loops are asymmetric, i.e. their apices are shifted toward one of the footpoints. This tendency is also confirmed by the computation of coronal magnetic fields based on the photospheric magnetic data.
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On leave from Observatoire de Paris-Meudon, 91190 Meudon, France.
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Berton, R., Sakurai, T. Stereoscopic determination of the three-dimensional geometry of coronal magnetic loops. Sol Phys 96, 93–111 (1985). https://doi.org/10.1007/BF00239795
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DOI: https://doi.org/10.1007/BF00239795