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Numerical computation results of the linear polarization parameters of the Ovi1031:92 coronal line are presented. They are based on theoretical results obtained by Raouafi (2002 and 2000), which give the Stokes parameters of a resonance scattering spectral line sensitive simultaneously to the Hanle eect and to the Doppler redistribution. In the present coronal case, the Hanle eect is due to the coronal magnetic field and the Doppler redistribution to the macroscopic motion of the scattering O 5+ coronal ions (solar wind velocity field vector). Constraints on the coronal magnetic field vector and on the solar wind velocity field vector are obtained by comparing the numerical results and the linear polarization measurements of the Ovi1031:92 coronal line obtained through particular observations performed by SUMER/SoHO.

Linear polarization of the $\ion{O}{iv}$λ1031.92 coronal line