Physics
Scientific paper
May 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984siva.work..121n&link_type=abstract
In NASA, Washington Solar Irradiance Variations on Active Region Time Scales p 121-123 (SEE N84-27635 17-92)
Physics
Mathematical Models, Solar Flux, Solar Magnetic Field, Solar Physics, Stellar Luminosity, Stellar Models, Faculae, Heat Transmission, Limb Brightening, Magnetohydrodynamics, Solar Flux Density, Solar Wind
Scientific paper
Changes in the local solar luminosity due to the presence of a small scale structured (facular) magnetic field in the photosphere are discussed. The discussion is based on three dimensional numerical simulations of the magnetohydrodynamics of the top of the convection zone, and the adjacent stable photosphere. The simulations demonstrate that practically all of the magnetic flux present is concentrated into intense magnetic flux structures, such that the magnetic field pressure is balanced by the gas pressure of the surrounding plasma. The flux concentration is caused by the convectively unstable stratification. The average luminosity of the area is influenced by three effects: (1) the brightness of the flux concentrations, (2) their filling factor, and (3) the average luminosity of the surrounding plasma.
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