The role of magnetic waves in tangent cylinder convection

TL;DR

This paper investigates how magnetic waves influence convection within the Earth's tangent cylinder, revealing their role in polar vortex formation and explaining observed geomagnetic variations through wave-driven upwellings.

Contribution

It demonstrates the significance of slow and fast magnetic-Archimedean-Coriolis waves in tangent cylinder convection and their impact on Earth's polar vortices, a novel insight into geomagnetic dynamics.

Findings

Slow MAC waves become comparable to fast MAC waves at specific frequency ratios.

Localized excitation of slow MAC waves drives upwellings in dynamo simulations.

Polar vortex strength correlates with the parity of wave intensities.

Abstract

The secular variation of the geomagnetic field suggests that there are anticyclonic polar vortices in the Earth's core. Under the influence of a magnetic field, the polar azimuthal flow is thought to be produced by one or more coherent upwellings within the tangent cylinder, offset from the rotation axis. In this study, convection within the tangent cylinder in rapidly rotating dynamos is investigated through the analysis of forced magnetic waves. The first part of the study investigates the evolution of an isolated buoyancy disturbance in an unstably stratified rotating fluid subjected to an axial magnetic field. It is shown that the axial flow intensity of the slow Magnetic-Archimedean-Coriolis (MAC) waves becomes comparable to that of the fast MAC waves when $|\omega_M/\omega_C| \sim 0.1$, where $\omega_M$ and $\omega_C$ are the Alfv\'en wave and inertial wave frequencies respectively. In spherical shell dynamo simulations, the isolated upwellings within the tangent cylinder are shown to originate from the localized excitation of slow MAC waves in the dipole-dominated regime. Axial flow measurements in turn reveal the approximate parity between the slow and fast wave intensities in this regime, which corresponds to the existence of strong polar vortices in the Earth's core. To obtain the observed peak azimuthal motions of $0.6$--$0.9^\circ$yr$^{-1}$, the Rayleigh number in the low-inertia geodynamo must be $\sim 10^3$ times the Rayleigh number for the onset of nonmagnetic convection. However, if the forcing is so strong as to cause polarity reversals, the field within the tangent cylinder decays away, and the convection takes the form of an ensemble of plumes supported entirely by the fast waves of frequency $\omega \sim \omega_C$. The resulting weak polar circulation is comparable to that obtained in nonmagnetic convection.