Radio and EUV observations of a coronal hole

Details Radio and EUV observations of a coronal hole Radio and EUV observations of a coronal hole

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...52..349d&link_type=abstract

Solar Physics, vol. 52, May 1977, p. 349-367.

Astronomy and Astrophysics

Astronomy

29

Density Distribution, Far Ultraviolet Radiation, Radio Astronomy, Solar Atmosphere, Solar Corona, Stellar Models, Temperature Distribution, Abundance, Atmospheric Models, Brightness Temperature, Nonequilibrium Ionization, Radio Telescopes, Stellar Structure, Thermal Diffusion

Scientific paper

Current ideas and modeling assumptions concerning the structure of the transition region and corona are summarized. Observations of a specific coronal hole are reported which were made with the EUV spectroheliometer aboard Skylab and with high-resolution radio telescopes in Australia and West Germany. Theoretical EUV line intensities and radio brightness temperatures are calculated, and an attempt is made to analyze the observations on the basis of standard one-dimensional plane-parallel hydrostatic-equilibrium models for the transition region and corona. It is found that any given standard model predicts either higher radio brightnesses or lower EUV line intensities than are observed. Several potential problem areas are examined in order to resolve this conflict. It is concluded that a model involving departures from hydrostatic equilibrium, varying conductive flux, mass outflow, as well as effects of thermal diffusion and nonequilibrium ionization should be investigated in more detail.

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