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Energy balance of stellar coronae. III - Effect of stellar mass and radiusA homologous transformation is derived which permits the application of the numerical coronal models of Hammer from a star with solar mass and radius to other stars. This scaling requires a few approximations concerning the lower boundary conditions and the temperature dependence of the conductivity and emissivity. These approximations are discussed and found to be surprisingly mild. Therefore, the scaling of the coronal models to other stars is rather accurate; it is found to be particularly accurate for main-sequence stars. The transformation is used to derive an equation that gives the maximum temperature of open coronal regions as a function of stellar mass and radius, the coronal heating flux, and the characteristic damping length over which the corona is heated.
Document ID
19840052301
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Hammer, R.
(Joint Institute for Laboratory Astrophysics, Boulder, CO; Heidelberg, Universitaet Heidelberg, Germany)
Date Acquired
August 12, 2013
Publication Date
May 15, 1984
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 280
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
84A35088
Funding Number(s)
CONTRACT_GRANT: DFG-SFB-132
CONTRACT_GRANT: NAG5-82
CONTRACT_GRANT: NGL-06-003-057
Distribution Limits
Public
Copyright
Other

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