Abstract
Molecular lines formed in the upper photosphere of the Sun show significant degree of linear scattering polarization, when one observes close to the solar limb. Those lines prove to be important tools for turbulent magnetic field diagnostic via the Hanle effect. In order to correctly model the line formation in regions close to the Solar limb, one has to take into account the sphericity of the atmosphere and to model depolarizing collisions and NLTE line formation in details. We present computations of scattering polarization in C2 lines in a 1D spherically symmetric medium described by FALC and FALX models, and compare those computations to observations of the Solar flash spectrum.
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