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This paper considers the problem of modeling the light polarization thatemerges from an astrophysical plasma composed of atoms whose excitation stateis significantly influenced by the anisotropy of the incident radiation field.In particular, it highlights how radiative transfer simulations inthree-dimensional models of the quiet solar atmosphere may help us to probe itsthermal and magnetic structure, from the near equilibrium photosphere to thehighly non-equilibrium upper chromosphere. The paper finishes with predictionsconcerning the amplitudes and magnetic sensitivities of the linear polarizationsignals produced by scattering processes in two transition region lines, whichshould encourage us to develop UV polarimeters for sounding rockets and spacetelescopes with the aim of opening up a new diagnostic window in astrophysics.

Modeling Scattering Polarization for Probing Solar Magnetism