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Problems of Solar Convection

Published online by Cambridge University Press:  19 July 2016

Wasaburo Unno
Wasaburo Unno*
Affiliation:
Research Institute for Science and Technology Kinki University 3-4-1 Kowakae, Higashi-Osaka-city, 577 Osaka Japan

Abstract

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Kinetic energy of convection is transported inwards in the main body of convection zone. The temperature gradient becomes super-radiative at the top of the overshooting zone. These two effects make the solar equilibrium model much less sensitive to the assumed mixing length in Xiong's eddy diffusion theory. Observed brightening of downflow at high level in the surface region over intergranular lanes seems to be consistent with the overshooting model. Momentum transport by convective motion is shown to be crucial in pushing down magnetic flux tubes against buoyancy. Also, subadiabatic layers are possibly formed temporarily in the middle of the convection zone, exciting oscillations and generating chaotic motions.

Type
II. The Solar Interior
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 39 - 44
Copyright
Copyright © Kluwer 1990 

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