TL;DR
This paper reviews the theory of planetary dynamos, emphasizing convection-driven magnetic field generation in planetary cores and discussing current limitations in understanding magnetic field variability and structure.
Contribution
It provides an overview of planetary dynamo theory and highlights the challenges in modeling magnetic field time dependence and toroidal components.
Findings
Convection flows are key to planetary magnetic field generation.
Current models are limited in explaining magnetic field variability.
Understanding of magnetic field structure remains incomplete.
Abstract
The theory of planetary dynamos and its applications to observed phenomena of planetary magnetism are outlined. It is generally accepted that convection flows driven by thermal or compositional buoyancy are the most likely source for the sustenance of global planetary magnetic fields. While the existence of dynamos in electrically conducting fluid planetary cores provides constraints on properties of the latter, the lack of knowledge about time dependences of the magnetic fields and about their toroidal components together with the restricted parameter regions accessible to theory have prevented so far a full understanding of the phenomena of planetary magnetism.
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