![The Stokes profiles of the Mg II k line calculated in a semi-empirical model of the solar atmosphere, in the absence (black curves) and in the presence (coloured curves) of a horizontal magnetic field with zero azimuth (i.e., on the plane defined by the l The Stokes profiles of the Mg II k line calculated in a semi-empirical model of the solar atmosphere, in the absence (black curves) and in the presence (coloured curves) of a horizontal magnetic field with zero azimuth (i.e., on the plane defined by the l](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/news/resultados178_194.jpg?itok=s4Gsddj9)
The polarization of the Mg II k line at 279.5 nm encodes valuable information on the magnetic field of the upper solar chromosphere, where this strong resonance line originates. We have developed a novel radiative transfer code which allows us to account for scattering polarization and the Hanle and Zeeman effects, as well as partial frequency redistribution (PRD) phenomena (i.e., correlation effects between the incoming and outgoing photons in the scattering events). This non-LTE code, which treats the atomic system and the polarized radiation field quantum-mechanically, has been applied to
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