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Energy balance in solar and stellar chromospheresNet radiative cooling rates for quiet and active regions of the solar chromosphere and for two stellar chromospheres are calculated from corresponding atmospheric models. Models of chromospheric temperature and microvelocity distributions are derived from observed spectra of a dark point within a cell, the average sun and a very bright network element on the quiet sun, a solar plage and flare, and the stars Alpha Boo and Lambda And. Net radiative cooling rates due to the transitions of various atoms and ions are then calculated from the models as a function of depth. Large values of the net radiative cooling rate are found at the base of the chromosphere-corona transition region which are due primarily to Lyman alpha emission, and a temperature plateau is obtained in the transition region itself. In the chromospheric regions, the calculated cooling rate is equal to the mechanical energy input as a function of height and thus provides a direct constraint on theories of chromospheric heating.
Document ID
19820051249
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Avrett, E. H.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 10, 2013
Publication Date
January 1, 1981
Subject Category
Astrophysics
Meeting Information
Meeting: In: Solar phenomena in stars and stellar systems
Location: Bonas
Country: France
Start Date: August 25, 1980
End Date: September 5, 1980
Accession Number
82A34784
Funding Number(s)
CONTRACT_GRANT: NSG-7054
Distribution Limits
Public
Copyright
Other

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