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The present work is on the study of a coronal streamer observed in March 2008at high spectral and spatial resolution by the Ultraviolet CoronagraphSpectrometer (UVCS) onboard SOHO. On the basis of a spectroscopic analysis ofthe O VI doublet, the solar wind plasma parameters are inferred in the extendedcorona. The analysis accounts for the coronal magnetic topology, extrapolatedthrough a 3D magneto-hydrodynamic model. The results of the analysis showindications on the formation of the current sheet, one of the source regions ofthe slow coronal wind.

Formation of the current sheet in a coronal streamer