Working Group 4 Report: Composition and Elemental Abundance Variations in the Solar Atmosphere and Solar Wind

Details Working Group 4 Report: Composition and Elemental Abundance Variations in the Solar Atmosphere and Solar Wind Working Group 4 Report: Composition and Elemental Abundance Variations in the Solar Atmosphere and Solar Wind

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ssrv...87..105m&link_type=abstract

Space Science Reviews, v. 87, Issue 1/2, p. 105-121 (1999).

Physics

3

Element Abundances, In Situ Observations, Uv Data

Scientific paper

This paper contains a summary of the topics treated in the working group on abundance variations in the solar atmosphere and in the solar wind. The FIP bias (overabundance of particles with low First Ionization Potentials over photospheric abundances) in coronal holes and coronal hole associated solar wind amounts to values between 1 and 2. The FIP bias in the slow solar wind is typically a factor 4, consistent with optical observations in streamers. In order to distinguish between different theoretical models which make an attempt to explain the FIP bias, some observable parameters must be provided. Unfortunately, many models are deficient in this respect. In addition to FIP fractionation, gravitational settling of heavy elements has been found in the core of long lived streamers. The so-called electron 'freeze in' temperatures derived from in situ observed ionization states of minor ions in the fast wind are significantly higher than the electron temperatures derived from diagnostic line ratios observed in polar coronal holes. The distinction between conditions in plumes and interplume lanes needs to be further investigated. The 'freeze in' temperatures for the slow solar wind are consistent with the electron temperatures derived for streamers.

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