Structure and physics of solar faculae

Details Structure and physics of solar faculae Structure and physics of solar faculae

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..138..213p&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 138, no. 2, April 1992, p. 213-222.

Physics

Carbon, Chromosphere, Faculae, Optical Thickness, Oxygen Spectra, Solar Corona, Line Spectra, Lyman Alpha Radiation, Solar Atmosphere, Solar Limb

Scientific paper

The optical depths of layers in the chromosphere-corona transition (CCT) zone, which is responsible for resolved structures in CII, CIII, OIV, and OVI lines, were determined using a new method that takes into account the effect of roughness (or local departures from sphericity) of the emitting layers in the CCT zone. The method allows determination of the angle alpha typical of the roughness (in case of availability of resolved data) and the two optical depths tau-1 and tau-2. It is shown that, even in unresolved cases, the new method gives a more realistic determination of the optical depths than previously determined.

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