Abstract
The slow solar wind is supposed to originate from coronal regions associated with streamers. It is not clear yet how the closed magnetic field structures of streamers are opening up in order to release the plasma. An analysis of this subject, particularly of a streamer on March 1998, is done using LASCO‐C1 spectral data. LASCO‐C1 is an internally occulted coronagraph on the SOHO spacecraft. It has a tunable Fabry‐Perot interferometer which allows taking spectral scans of selected coronal emission lines. From measured line profiles we deduced physical quantities like temperature and flow velocities along the line of sight. This way, we obtained information on the flow pattern in the low corona.
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