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The plasma thermodynamics in the solar upper atmosphere, particularly in thecorona, are dominated by the magnetic field, which controls the flow anddissipation of energy. The relative lack of knowledge of the coronal vectormagnetic field is a major handicap for progress in coronal physics. This makesthe development of measurement methods of coronal magnetic fields a highpriority in solar physics. The Hanle effect in the UV and IR spectral lines isa largely unexplored diagnostic. We use magnetohydrodynamic (MHD) simulationsto study the magnitude of the signal to be expected for typical coronalmagnetic fields for selected spectral lines in the UV and IR wavelength ranges,namely the H I Ly-$\alpha$ and the He I 10830 {\AA} lines. We show that theselected lines are useful for reliable diagnosis of coronal magnetic fields.The results show that the combination of polarization measurements of spectrallines with different sensitivities to the Hanle effect may be most appropriatefor deducing coronal magnetic properties from future observations.

Diagnostics of Coronal Magnetic Fields Through the Hanle Effect in UV and IR Lines