Temperature and density structure of the corona and inner solar wind

Details Temperature and density structure of the corona and inner solar wind Temperature and density structure of the corona and inner solar wind

Dec 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....53..363k&link_type=abstract

Astronomy and Astrophysics, vol. 53, no. 3, Dec. 1976, p. 363-375.

Astronomy and Astrophysics

Astrophysics

35

Density Distribution, Solar Corona, Solar Wind, Stellar Models, Temperature Distribution, Energy Dissipation, Energy Spectra, Fine Structure, Magnetic Field Configurations, Radial Distribution, Radiative Transfer, Solar Spectra, Stellar Structure, Thermal Conductivity, Ultraviolet Spectra

Scientific paper

A combined theoretical and observational approach is used to construct models of the inner corona applicable to quiet open-field regions and coronal holes. These models, extending from the top of the transition region at about 1.003 solar radii out to 3 solar radii, are calculated by employing parameters that describe the coronal geometry and heating. Thermal conductivity, heating, radiative losses, and solar-wind convection are included in the full energy-balance equation, which is integrated to obtain density and temperature models; the unknown heating term is parameterized in terms of the mechanical flux incident at the base and the characteristic scale height for the dissipation of this flux; and boundary conditions at the base are fixed by EUV-derived models of the transition region. Two representative models, one for a coronal hole and one for a quiet region, are examined in detail as illustrative examples of the technique used. It is noted that the models obtained predict most of the pertinent observations reasonably well but significantly overestimate the radio emission at 80 and 160 MHz and significantly underestimate the intensity of the Fe XV line at 284 A, especially in coronal holes.

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