The streamer boundary and the source of the slow wind

Details The streamer boundary and the source of the slow wind The streamer boundary and the source of the slow wind

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..477a&link_type=abstract

In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze

Physics

7

Solar Physics, Soho, Solar Wind

Scientific paper

The source of the slow solar wind that dominates the low latitude heliosphere during the minimum of solar activity has not yet been fully identified. We present preliminary results of a study concerning the streamer boundary regions in order to investigate the streamer-wind transition in the extended corona. The coronal plasma physical conditions, such as kinetic temperature of ions, electron density, abundance of oxygen and outflow velocity, are determined across the boundary of streamers. The study, based on data obtained with the Ultraviolet Coronagraph Spectrometers (UVCS) onboard SOHO, concern streamers observed at mid-low latitudes in the years 1996 and 1997, during the recent solar minimum. The analysis is based on ad-hoc diagnostic techniques developed to obtain the solar wind velocity, the electron density and the oxygen abundance of the extended corona, based on the O VI 1032, 1037 Å and the H I Ly&alpha 1216 Å lines.

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