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Structure and physics of solar faculae. II - The non-thermal velocity field above faculaeThe 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.
Document ID
19820052647
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Mouradian, Z.
(Paris, Observatoire, Meudon Hauts-de-Seine, France)
Dumont, S.
(Observatoire de Paris-Meudon France)
Pecker, J.-C.
(College de France Paris, France)
Chipman, E.
(NASA Headquarters Washington, DC United States)
Artzner, G. E.
(Observatoire de Paris-Meudon France)
Vial, J. C.
(CNRS, Laboratoire de Physique Stellaire et Planetaire, Verrieres-le-Buisson Essonne, France)
Date Acquired
August 10, 2013
Publication Date
May 1, 1982
Publication Information
Publication: Solar Physics
Volume: 78
Subject Category
Solar Physics
Accession Number
82A36182
Funding Number(s)
CONTRACT_GRANT: CNRS-RCP-310
Distribution Limits
Public
Copyright
Other

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