Convective Differential Rotation in Stars and Planets I: Theory

Abstract

We derive the scaling of differential rotation in both slowly- and rapidly-rotating convection zones using order of magnitude methods. Our calculations apply across stars and fluid planets and all rotation rates, as well as to both magnetized and purely hydrodynamic systems. We find shear $|R\nabla \Omega |$ of order the angular frequency $\Omega$ for slowly-rotating systems with $\Omega \ll |N|$, where $N$ is the \brvs\ frequency, and find that it declines as a power-law in $\Omega$ for rapidly-rotating systems with $\Omega \gg |N|$. We further calculate the meridional circulation rate and baroclinicity and examine the magnetic field strength in the rapidly rotating limit. Our results are in general agreement with simulations and observations and we perform a detailed comparison with those in a companion paper.

arXiv comment26 pages, 3 figures. Accepted in MNRAS. Comments welcome

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Cited by in corpus (3)

• Differential Rotation in a 3D Simulation of Oxygen Shell Burning
• Convective Differential Rotation in Stars and Planets II: Observational and Numerical Tests
• The rotational influence on solar convection