The chromosphere and transition regionThe physical processes occurring as a result of the transfer of energy and momentum from the primary solar flare energy release site in the corona to the underlying chromosphere and transition region during the course of the flare are investigated through a comparison of theoretical models and observational data. Static, dynamic and hydrodynamic models of the lower-temperature chromospheric flare are reviewed. The roles of thermal conduction, radiation, fast particles and mass motion in chromosphere-corona interactions are analyzed on the basis of Skylab UV, EUV and X-ray data, and empirical and synthetic models of the chromospheric and upper photospheric responses to flares are developed. The canonical model of chromospheric heating during flares as a result of primary energy release elsewhere is found to be justified in the chromosphere as a whole, although not entirely as the temperature minimum, and a simplified model of horizontal chromospheric flare structure based on results obtained is presented.
Document ID
19800052861
Acquisition Source
Legacy CDMS
Document Type
Other - Collected Works
Authors
Canfield, R. C. (California, University La Jolla, Calif., United States)
Brown, J. C. (California Univ. La Jolla, CA, United States)
Craig, I. J. D. (Glasgow, University Glasgow, United Kingdom)
Brueckner, G. E. (California Univ. La Jolla, CA, United States)
Cook, J. W. (California Univ. La Jolla, CA, United States)
Doschek, G. A. (U.S. Navy, Naval Research Laboratory, Washington D.C., United States)
Emslie, A. G. (California Univ. La Jolla, CA, United States)
Machado, M. E. (Harvard-Smithsonian Center for Astrophysics Cambridge, Mass., United States)