Characterization of the slow wind in the outer corona

Abstract

The study concerns the streamer belt observed at high spectral resolution during the minimum of solar cycle 22 with the Ultraviolet Coronagraph Spectrometer (UVCS) onboard SOHO. On the basis of a spectroscopic analysis of the O VI doublet, the solar wind plasma parameters are inferred in the extended corona. The analysis accounts for the coronal magnetic topology, extrapolated through a 3D magneto-hydrodynamic model, in order to define the streamer boundary and to analyse the edges of coronal holes. The results of the analysis allow an accurate identification of the source regions of the slow coronal wind that are confirmed to be along the streamer boundary in the open magnetic field region.

5 figures, work presented with an oral presentation on 37th COSPAR Scientific Assembly, 13 - 20 July 2008, Montreal, Canada

References in corpus (1)

• Why is the Fast Solar Wind Fast and the Slow Solar Wind Slow? A Survey of Geometrical Models

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