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A formulation of convection for stellar structure and evolution calculations without the mixing-length theory approximations. I - Application to the sunThe problem of treating convective energy transport without MLT approximations is approached here by formulating the results of numerical simulations of convection in terms of energy fluxes. This revised treatment of convective transport can be easily incorporated within existing stellar structure codes. As an example, the technique is applied to the sun. The treatment does not include any free parameters, making the models extremely sensitive to the accuracy of the treatments of opacities, chemical abundances, treatments of the solar atmosphere, and the equation of state.
Document ID
19930026512
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Lydon, Thomas J.
(NASA Headquarters Washington, DC United States)
Fox, Peter A.
(NASA Headquarters Washington, DC United States)
Sofia, Sabatino
(Yale Univ. New Haven, CT, United States)
Date Acquired
August 15, 2013
Publication Date
October 1, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 397
Issue: 2
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
93A10509
Funding Number(s)
CONTRACT_GRANT: NGT-50651
Distribution Limits
Public
Copyright
Other

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