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In order to obtain empirical information on the magnetism of the solartransition region we need to measure and interpret the linear polarizationproduced by scattering processes in FUV and EUV spectral lines. Via the Hanleeffect such linear polarization signals are sensitive to the magnetic fieldsexpected for the quiet and active regions of the outer solar atmosphere. Forexample, the Ly$\alpha$ line of H\,{\sc i} at 1216\,\AA\ is mainly sensitive tomagnetic strengths between 10 and 100 G. The interpretation of the observedspectral line polarization requires the development of suitable modeling tools.To this end, we have developed a three-dimensional (3D), non-LTE multilevelradiative transfer code for modeling the intensity and linear polarizationproduced by scattering processes in spectral lines and its modification by theHanle effect.

A 3D Radiative Transfer Code for Modeling the Hanle Effect in the Lyman-alpha line