Spectroscopic techniques for determining electron densities in the solar atmosphere

Details Spectroscopic techniques for determining electron densities in the solar atmosphere Spectroscopic techniques for determining electron densities in the solar atmosphere

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jphys..49...13m&link_type=abstract

(IAU, ESA, CNRS, et al., Colloquium on UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas, 102nd, Beaulieu-sur-Me

Physics

14

Electron Density (Concentration), Line Spectra, Solar Activity, Solar Atmosphere, Solar Physics, Electron Scattering, Solar Corona, Ultraviolet Spectra

Scientific paper

An account is given of methods for the determination of solar atmosphere electron densities, with emphasis on the atomic parameters required for such analyses and the approximations applicable in the calculation of electron scattering cross-sections. These techniques have shown the solar atmosphere's transition region to possess unresolved filamentary structures with very small filling factors at low temperatures. The coronal emission seems, by contrast, to be more homogeneously distributed. Significant results have also emerged from the study of solar flare electron densities.

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