![Left: Chromospheric image of a chromospheric active region at -161 mÅ from the core of the Ca II 8542 line, where fibrils are covering almost the entire field-of-view. Right: Circular polarization image (Stokes V) at the same wavelength, quantifies the st Left: Chromospheric image of a chromospheric active region at -161 mÅ from the core of the Ca II 8542 line, where fibrils are covering almost the entire field-of-view. Right: Circular polarization image (Stokes V) at the same wavelength, quantifies the st](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/news/resultados77_81.jpg?itok=Ws9mbqh4)
Fibrils are thin elongated features visible in the solar chromosphere in and around magnetized regions. Because of their visual appearance they have been traditionally considered a tracer of the magnetic field lines. To our best knowledge, this common conception has never been actually put to test, probably because a proper empirical determination of the chromospheric magnetic field is very challenging, requiring high-resolution spectro-polarimetry in chromospheric lines. In this work we challenge that notion for the first time by comparing their orientation to that of the magnetic field
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