Physics
Scientific paper
Jan 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982stin...8218113e&link_type=abstract
Unknown
Physics
Convection, Energy Transfer, Perturbation, Radii, Solar Activity, Solar Physics, Stellar Luminosity, Stellar Magnitude, Sun, Adiabatic Conditions, Atmospheric Models, Depth, Irradiance, Solar Oscillations, Stellar Evolution
Scientific paper
The response of solar models to perturbations of the efficiency of convective energy transport is studied for a number of cases. Such perturbations primarily effect the shallow superadiabatic layer of the convective envelope (at depth of approx. 1000 km below the photosphere). Independent of the details of the perturbation scheme, the resulting change in the solar radius is always very small compared to the change in luminosity. This appears to be true for any physical mechanism of solar variability which operates in the outer layers of the convection zone. Changes of the solar radius have been inferred from historical observations of solar eclipses. Considering the constraints on concurrent luminosity changes, this type of solar variability must be indicative of changes in the solar structure at substantial depths below the superadiabatic layer of the convective envelope.
Endal Andrew S.
Twigg Laurence W.
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