Hydromagnetic quasi-geostrophic modes in rapidly rotating planetary cores

Abstract

The core of a terrestrial-type planet consists of a spherical shell of rapidly rotating, electrically conducting, fluid. Such a body supports two distinct classes of quasi-geostrophic eigenmodes: fast, primarily hydrodynamic, inertial modes with period related to the rotation time scale and slow, primarily magnetic, magnetostrophic modes with much longer periods. Here, we investigate the properties of these hydromagnetic quasi-geostrophic modes as a function of non-dimensional parameters controlling the strength of the background magnetic field, the planetary rotation rate, and the amount of magnetic dissipation. ... read full length abstract in the paper.

References in corpus (3)

• Axial invariance of rapidly varying diffusionless motions in the Earth's core interior
• Elliptical instability in terrestrial planets and moons
• Observation of magnetocoriolis waves in a liquid metal Taylor-Couette experiment

Cited by in corpus (7)

• First evidence of inertial modes in $\gamma$ Doradus stars: The core rotation revealed
• The interplay of fast waves and slow convection in geodynamo simulations nearing Earth's core conditions
• Fast Quasi-Geostrophic Magneto-Coriolis Modes in the Earth's core
• Variability modes in core flows inverted from geomagnetic field models
• Pressure torque of torsional Alfvén modes acting on an ellipsoidal mantle
• Spatial And Temporal Changes Of The Geomagnetic Field: Insights From Forward And Inverse Core Field Models
• Characterisation of hydromagnetic waves propagating over a steady, non-axisymmetric background magnetic field