Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...297..787d&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 297, Oct. 15, 1985, p. 787-798.
Astronomy and Astrophysics
Astrophysics
20
Convective Flow, Solar Rotation, Solar Simulation, Stellar Cores, Turbulent Flow, Angular Momentum, Dynamo Theory
Scientific paper
It is shown that the time rate of change (brought about by the turbulent convective motions) in the angular momentum of a thin spherical shell of radius r is such as to increase the angular velocity of the lower part (τΩ0 > 1; τ is the dominant eddy's lifetime) of the solar convection zone (SCZ) and to decrease the angular velocity of the upper part (τΩ0 < 1). A tentative model of rotation in the SCZ is proposed: (1) the (τΩ0 > 1)-region is in weaker differential rotation than the surface and not constrained by the Taylor-Proudman theorem, (2) the observed solar differential rotation at the surface is then generated as the SCZ relaxes from the (τΩ0 > 1)-state in the lower part to the (τΩ0 < 1)-state at the surface. In the upper and lower layers of the SCZ, angular-momentum conservation between the turbulent motions and viscous stresses leads to an angular velocity increasing inward.
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