The emission-line spectrum above the limb of a solar coronal hole - 1175-1940 A

Details The emission-line spectrum above the limb of a solar coronal hole - 1175-1940 A The emission-line spectrum above the limb of a solar coronal hole - 1175-1940 A

Jul 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apjs...31..445f&link_type=abstract

Astrophysical Journal Supplement Series, vol. 31, July 1976, p. 445-466. NASA-supported research.

Astronomy and Astrophysics

Astronomy

80

Line Spectra, Solar Corona, Solar Limb, Solar Spectra, Ultraviolet Spectra, Skylab Program, Spaceborne Astronomy, Spectroheliographs

Scientific paper

Emission-line spectra of a coronal hole that coincided with the north pole of the sun are discussed which were obtained with a slit spectrograph aboard Skylab at positions within and above the solar white-light limb in the wavelength range from 1175 to 1940 A. Relative line intensities, line profiles, and full widths at half-maximum are presented for selected chromospheric and transition-zone lines observed above the present polar coronal hole. Average mass motions in the transition zone are determined as a function of electron temperature from the widths of the optically thin lines by assuming ionization equilibrium. The line intensities and profiles are compared with corresponding results deduced from spectra obtained above a quiet solar region. The coronal-hole spectra are found to imply an angular dependence for the source function as well as a radial dependence such that the source function is the smallest at the south pole and increases with decreasing solar latitude.

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