Physics
Scientific paper
Oct 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...54..363r&link_type=abstract
Solar Physics, vol. 54, Oct. 1977, p. 363-370.
Physics
Chromosphere, Far Ultraviolet Radiation, Line Spectra, Solar Atmosphere, Temperature Effects, Ultraviolet Spectroscopy, Atmospheric Temperature, Electron Transitions, Emission Spectra, Spectral Resolution
Scientific paper
Consequences of the complex emission network characteristic of the chromosphere for medium-resolution EUV observations are investigated. Observed correlations are discussed between the intensity of the Mg X line at 625 A and the line intensities of N V at 1239 A, O VI at 1032 A, Ne VIII at 770 A, Na IX at 682 A, Al XI at 550 A, and Si XII at 449 A. Certain discontinuities in the intensity correlations are analyzed, the fractional emitting areas for N V, O VI, and Ne VIII are computed as a function of temperature, and the height variation of the fractional emitting areas is examined. The results show that: (1) the fractional emitting area increases with increasing temperature in the transition region for most values of Mg X intensity; (2) the fractional emitting area decreases with increasing Mg X intensity for a fixed temperature, indicating that the relevant temperature is reached at a lower height; and (3) both the average fractional area and the width of a typical network element increase only slightly with temperature.
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