EUV spectroscopic plasma diagnostics for the solar wind acceleration region

Details EUV spectroscopic plasma diagnostics for the solar wind acceleration region EUV spectroscopic plasma diagnostics for the solar wind acceleration region

May 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...256..263k&link_type=abstract

Astrophysical Journal, Part 1, vol. 256, May 1, 1982, p. 263-270. Research supported by the Smithsonian Institution;

Physics

Optics

76

Plasma Acceleration, Plasma Diagnostics, Solar Corona, Solar Spectra, Solar Wind, Ultraviolet Spectroscopy, Abundance, Coronagraphs, Extreme Ultraviolet Radiation, Ion Temperature, Mass Flow Rate, Particle Flux Density, Plasma Density, Plasma Temperature, Resonance Lines, Solar Electrons, Solar Protons, Solar Wind Velocity, Spectral Line Width

Scientific paper

Possibilities are considered for probing physical conditions in the solar corona with strong EUV resonance lines from ions such as N V, O VI, Ne VIII, Mg X, and Si XII. Through measurements of the intensities and profiles of EUV spectral lines with coronagraphic instrumentation employing normal incidence reflecting optics, it is possible to acquire information on electron, proton, and ion temperatures and velocity distributions; electron, H I, and ion densities; mass flow and nonthermal velocities; and chemical abundances. This information will provide critical empirical constraints on physical processes responsible for plasma heating, solar wind acceleration, and transport of mass, momentum, and energy in the solar corona, as well as providing constraints on theoretical models for solar and stellar coronae and mass loss.

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