Variations of Strahl Properties With Fast and Slow Solar Wind

Details Variations of Strahl Properties With Fast and Slow Solar Wind Variations of Strahl Properties With Fast and Slow Solar Wind

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh21a1578n&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH21A-1578

Physics

2164 Solar Wind Plasma

Scientific paper

The interplanetary solar wind electron velocity distribution function generally shows three different populations. Two of the components, the core and halo, have been the most intensively analyzed and modeled populations using different theoretical models. The third component, the strahl, is usually seen at higher energies, is confined in pitch-angle, is highly field-aligned and skew. This population has been more difficult to identify and to model in the solar wind. In this work we make use of the high angular, energy and time resolution and three-dimensional data of the Cluster/PEACE electron spectrometer to identify and analyze this component in the ambient solar wind during high and slow speed solar wind. The moment density and fluid velocity have been computed by a semi-numerical integration method. The variations of solar wind density and drift velocity with the general bulk solar wind speed could provide some insight into the source, origin, and evolution of the strahl.

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