Coronal holes are known to be the source of the fast, relatively homogeneous solar wind. A more variable slow solar wind emerges from the corona adjacent to these fast streams and dominates the low latitude heliosphere during the minimum of solar activity. The objective of this paper is the study of the coronal hole-streamer interface and of the physical conditions (i.e. kinetic temperature of oxygen ions, abundance of oxygen, outflow velocity) inside and at the boundary of a streamer, in order to investigate the source of the slow solar wind. The data used in the analysis are obtained with the Ultraviolet Coronagraph Spectrometer (UVCS) onboard SOHO and concern streamers at mid-low latitudes observed in 1996, during the solar minimum.
Solspa 2001, Proceedings of the Second Solar Cycle and Space Weather Euroconference
- Pub Date:
- March 2002
- Solar Physics;
- Slow Solar Wind