2012/05/14 by Jiří Štěpán, J. Trujillo Bueno, Stepan, Jiri +1
Physics and Astronomy · #Astronomy and Astrophysical Research #FOS: Physical sciences #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.1205.2959
openalex publication_date 2012/05/14 · openalex created_date 2022/10/01 · openalex updated_date 2026/07/28
In order to obtain empirical information on the magnetism of the solar\ntransition region we need to measure and interpret the linear polarization\nproduced by scattering processes in FUV and EUV spectral lines. Via the Hanle\neffect such linear polarization signals are sensitive to the magnetic fields\nexpected for the quiet and active regions of the outer solar atmosphere. For\nexample, the Ly\α line of H , sc i at 1216 , AA is mainly sensitive to\nmagnetic strengths between 10 and 100 G. The interpretation of the observed\nspectral line polarization requires the development of suitable modeling tools.\nTo this end, we have developed a three-dimensional (3D), non-LTE multilevel\nradiative transfer code for modeling the intensity and linear polarization\nproduced by scattering processes in spectral lines and its modification by the\nHanle effect.\n