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The temperature structure, mass, and energy flow in the corona and inner solar windRemote-sensing and in situ data are used to constrain a radiative energy balance model in order to study the radial variations of coronal temperatures, densities, and outflow speeds in several types of coronal holes and in an unstructured quiet region of the corona. A one-fluid solar wind model is used which takes into account the effects of radiative and inward conductive losses in the low corona and the chromospheric-coronal transition region. The results show that the total nonradiative energy input in magnetically open coronal regions is 5 + or - 10 to the 5th ergs/sq cm, and that most of the energy heating the coronal plasma is dissipated within 2 solar radii of the solar surface.
Document ID
19880041521
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Withbroe, George L.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 13, 2013
Publication Date
February 1, 1988
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 325
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
88A28748
Funding Number(s)
CONTRACT_GRANT: NAGW-249
Distribution Limits
Public
Copyright
Other

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