Structure and physics of solar faculae. III - The densities in the chromosphere-corona transition zone

Details Structure and physics of solar faculae. III - The densities in the chromosphere-corona transition zone Structure and physics of solar faculae. III - The densities in the chromosphere-corona transition zone

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...83...27d&link_type=abstract

Solar Physics, vol. 83, Feb. 1983, p. 27-50. Research supported by the Centre National d'Etudes Spatiales; Centre National de la

Physics

10

Faculae, Resonance Lines, Solar Spectra, Calibrating, Carbon, Electron Density (Concentration), Opacity, Oso-8, Oxygen Spectra, Silicon

Scientific paper

Si Iv, C Iv, and 0 vI resonance lines have been measured above quiet and active solar regions from both pointed OSO-8 instruments. From calibrated profiles, optical depths are computed with three different methods. All three methods provide evidence that the opacity above faculae is lower than above the quiet Sun. From lower and upper limits of the opacity, we derive limits of the electron density. Our first method assumes only that the source function is constant without any geometrical constraint. We find higher densities above faculae than above quiet regions (about a factor 10). A second method allows us to compute the density, temperature gradient and thickness of a plane-parallel model, for active and quiet Sun. Electron densities agree with those of the first method but they lie in the lower range of values previously determined from Skylab. This result can be explained by the moderate level activity of the observed faculae. Appendices give relevant elements of transfer theory and newly computed values of collisional rates.

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