Other
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..193v&link_type=abstract
Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 193
Other
5
Particle Emission, Solar Wind, Solar Instruments, Composition
Scientific paper
The abundances and charge states of the heavy ions present in the solar wind are important tracers for conditions and processes in the solar corona and chromosphere. The elemental abundances are known to be fractionated with respect to the photosphere, with the fractionation being organized best by the first ionization time. Since the first ionization occurs in the upper the chromosphere, the solar wind abundances are indicative for the conditions at this site. On the other hand, the solar wind charge states provide information about the coronal temperature, where they are frozen-in at altitudes between 1.5 and 3.5 solar radii. The charge state distributions of different elements can thus be used to infer a coronal temperature profile. The two types of steady solar wind, fast streams from coronal holes and slow, interstream wind, are significantly different in both of these signatures. This implies that they are separated by a boundary extending through the corona and down into the chromosphere, i.e. that the slow wind is not merely emanating from the coronal hole boundary regions.
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