The intensities and profiles of XUV transition zone lines in a quiet sun region compared to a polar coronal hole

Details The intensities and profiles of XUV transition zone lines in a quiet sun region compared to a polar coronal hole The intensities and profiles of XUV transition zone lines in a quiet sun region compared to a polar coronal hole

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...202l.147f&link_type=abstract

Astrophysical Journal, vol. 202, Dec. 15, 1975, pt. 2, p. L147-L150. NASA-supported research.

Astronomy and Astrophysics

Astrophysics

28

Chromosphere, Far Ultraviolet Radiation, Solar Atmosphere, Solar Corona, Electron Transitions, Polar Regions, Radiant Flux Density, Solar Activity, Solar Limb, Solar Spectra, Velocity Measurement

Scientific paper

The intensities of XUV transition-zone lines from limb spectra of a quiet-sun region and a polar coronal hole are compared. The spectra were obtained with a slit spectrograph on Skylab and cover a region from -12 sec within the limb to 20 sec above it. The lines selected for comparison are formed at temperatures that range from 36,000 to 220,000 K. Lines of the higher-temperature ions, e.g. O v, are significantly less intense in the coronal hole, and lines of lower-temperature ions show little change. Profiles of selected optically thin transition-zone lines from the quiet-sun and coronal-hole spectra are also shown. The lines are broader than expected in ionization equilibrium, and bulk-motion velocities are deduced from the widths of the lines. There appears to be little, if any, statistically significant difference in the velocities obtained from the quiet-sun region and the coronal hole.

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