Structure and physics of solar faculae. II - The non-thermal velocity field above faculae

Details Structure and physics of solar faculae. II - The non-thermal velocity field above faculae Structure and physics of solar faculae. II - The non-thermal velocity field above faculae

May 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...78...83m&link_type=abstract

Solar Physics, vol. 78, May 1982, p. 83-100. Research supported by the Centre National d'Etudes Spatiales; Centre National de la

Physics

9

Faculae, Solar Physics, Velocity Distribution, Chromosphere, Line Spectra, Oso-8, Solar Corona, Solar Spectra, Stellar Structure

Scientific paper

The OSO-8 satellite enabled the study of various characteristics of the profiles of Si II, Si IV, C IV, and O VI lines above active areas of the sun, as well as above quiet areas, and the derivation of some physical properties of the transition region between chromosphere and corona (CCT). The study of the lines shows a general tendency for the microvelocity fields on the average to be nearly constant for the heights corresponding to a temperature greater than 100,000 K; however they seem to slightly increase with height in quiet areas, and decrease in active areas. A multicomponent model of the CCT is necessary, and its geometry is far from being a set of plane-parallel columns. It is similar to an association of moving knots within the nonmoving principal component of the matter. The proportion of mass, in the knots relative to that in the nonmoving component, is several times larger in active regions than in quiet regions. In the knots, the nonthermal microvelocity fields are smaller in active regions and seem to decrease for temperature increasing above 100,000 K, contrary to what happens in the steady principal component.

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