Titlebook: Solar Phenomena in Stars and Stellar Systems; Proceedings of the N Roger M. Bonnet,Andrea K. Dupree Conference proceedings 1981 D. Reidel P

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Compressible Convection in a Rotating Spherical Shellvation is to understand the maintenance of the two major ingredients in solar dynamo theory, that is helicity and differential rotation. An anelastic approximation filters out sound waves but permits the investigation of the effects of large density stratifications in slightly superadiabatic stellar

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Magnitude

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Coronal Holes and Solar Mass Loss. These streams originate in low density, low temperature coronal regions, called “holes.” The physical properties of the wind streams and the holes will be discussed. Preliminary models for the three-dimensional structure of the wind, at different phases of the solar activity cycle, will be sketche

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CANDY

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Compressible Convection in a Rotating Spherical Shellon of the most unstable modes decreases, the prograde phase velocity increases, and the buoyancy force does more negative work in the upper part of the convection zone. Differential rotation is maintained by the transport of longitudinal momentum and by the coriolis forces acting on the meridional c