Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...276..316h&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 1, 1984, p. 316-324.
Astronomy and Astrophysics
Astrophysics
30
Astrophysics, Convection, Mixing Length Flow Theory, Rotating Fluids, Stellar Models, Turbulence Models, Turbulent Mixing, Dynamo Theory, Hydrodynamics, Stellar Structure, Stress Tensors, Vortices
Scientific paper
The effects of rotation are included in an analytical model for the convective motions in a plane-parallel layer of an ideal fluid. The turbulent stress tensor, formed by taking products and averages of the various velocity components, is calculated for an arbitrary eddy size and shape. Heuristic formulae presented for determining the size and shape of the dominant eddy then give a fully specified stress tensor. Applications for this stress tensor in problems of stellar internal dynamics, heat flow, scalar diffusion, and dynamo theory are suggested. The resultant stresses tend to produce differential rotation profiles with rapidly rotating equators and interiors. The dynamo activity associated with these convective motions tends to occur near the lower boundary of the convection zone.
No associations
LandOfFree
A convective model for turbulent mixing in rotating convection zones does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with A convective model for turbulent mixing in rotating convection zones, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A convective model for turbulent mixing in rotating convection zones will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-935905