Probing the solar wind acceleration region using spectroscopic techniques

Details Probing the solar wind acceleration region using spectroscopic techniques Probing the solar wind acceleration region using spectroscopic techniques

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ssrv...33...17w&link_type=abstract

(Lindau Workshop on the Source Region of the Solar Wind, 9th, Lindau, West Germany, Nov. 1981.) Space Science Reviews, vol. 33,

Computer Science

Sound

129

Plasma Acceleration, Solar Spectra, Solar Wind Velocity, Ultraviolet Spectroscopy, Abundance, Electron Scattering, Line Spectra, Lyman Alpha Radiation, Rocket-Borne Instruments, Solar Corona, Solar Radiation, Velocity Distribution

Scientific paper

Recent developments in the use of UV and EUV coronagraphic spectroscopy for studying the physical conditions in the solar corona in the solar wind acceleration region from a heliocentric distance of 1.8 solar radii out to 8 solar radii and beyond are reviewed. Particular attention is given to theoretical considerations and techniques for the estimation of particle ionization balances and velocity distributions, coronal temperatures, neutral hydrogen, proton, electron and ion temperatures and densities, outflow velocities, charge states and chemical abundances from spectral line radiation and white-light measurements. Observational considerations are discussed as they relate to requirements for stray light rejection and the effects of geocorona and interplanetary dust emission in coronagraph design. Results of coronal H I Lyman alpha and white light observations made during sounding rocket flights are summarized, and future observational programs making use of rocket-borne instruments, Detached Shuttle Payload Flights, Spacelab or space platforms are indicated.

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