Zonal-mean atmospheric dynamics of slowly-rotating terrestrial planets

TL;DR

This paper investigates the atmospheric dynamics of slowly-rotating terrestrial planets using numerical simulations and theoretical models, revealing how low rotation rates influence zonal wind, temperature profiles, and overturning circulation.

Contribution

It compares two zonally symmetric theories with numerical simulations, showing how overturning circulation smooths temperature and wind profiles at low planetary rotation rates.

Findings

Numerical simulations show smoother temperature profiles than theoretical models.

Zonal wind at the poles decreases with planetary rotation rate, collapsing at zero rotation.

Eddy motions in 3D simulations align more with the variant theoretical model.

Abstract

The zonal-mean atmospheric flow of an idealized terrestrial planet is analyzed using both numerical simulations and zonally symmetric theories, focusing largely on the limit of low planetary rotation rate. Two versions of a zonally symmetric theory are considered, the standard Held-Hou model, which features a discontinuous zonal wind at the edge of the Hadley cell, and a variant with continuous zonal wind but discontinuous temperature. The two models have different scalings for the boundary latitude and zonal wind. Numerical simulations are found to have smoother temperature profiles than either model, with no temperature or velocity discontinuities even in zonally symmetric simulations. Continuity is achieved because of the presence of an overturning circulation poleward of the point of maximum zonal wind, which allows the zonal velocity profile to be smoother than the original theory without the temperature discontinuities of the variant theory. Zonally symmetric simulations generally fall between the two sets of theoretical scalings, and have a faster polar zonal flow than either. Three-dimensional simulations that allow for eddy motion fall closer to the scalings of the variant model. At very low rotation rates the maximum zonal wind falls with falling planetary rotation rate, even in the three-dimensional simulations, and collapses completely at zero rotation. Nevertheless, the low-rotation limit of the overturning circulation is strong enough to drive the temperature profile close to a state of nearly constant potential temperature.