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Models of transition region and coronal plasma in solar loop structuresThe theory of coronal loops was developed and the simple version of the theory and observations are compared. It is shown that the gross properties of the confined corona can be understood by considering simple hydrostatic equilibrium models. By observing the corona it is apparent that hydrostatic models are seriously inadequate. It is suggested that observations of intensity fluctuations, of persistent up and down flows, of relatively cool matter residing at coronal heights, of apparent spatial co-mingling of hot plasmas at quite different temperatures, need a more sophisticated modeling.
Document ID
19830012577
Document Type
Conference Paper
Authors
Raymond, J. C. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Rosner, R. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 11, 2013
Publication Date
January 1, 1981
Publication Information
Publication: Smithsonian Astrophysics Observatory 2nd Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, Vol. 1
Subject Category
SOLAR PHYSICS
Funding Number(s)
CONTRACT_GRANT: NAS5-3949
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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IDRelationTitle19830012575Analytic PrimarySecond Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, volume 1