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Local and Non-Local Contributions to Horizontal Motions in Stellar Convective Zones
Published online by Cambridge University Press: 12 April 2016
Abstract
A method to determine the r.m.s. horizontal velocities in stellar convective zones (assuming that non-locality effects are not too strong) is given and applied to the solar case. The results may serve as useful input parameters for both convection theory and dynamo theory.
- Type
- III. Input physics for stellar structure
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- Copyright © Astronomical Society of the Pacific 1993