Planetary Magnetic Fields and Fluid Dynamos

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Anelastic convection-driven dynamo benchmarks (2011, unknown): “Although the Ekman number is 2 10 (3), and so not very small compared with recently published Boussinesq dynamos (Kageyama et al., 2008; Sakuraba and Roberts, 2009; Jones, 2011) the convection is still columnar as can be seen in Fig.”
Rotating convective turbulence in Earth and planetary cores (2015, methodology): “(For detailed descriptions of magnetic induction processes in planetary dynamos and numerical dynamo models, we refer to a number of recent review articles: Sreenivasan (2010), Jones (2011), Roberts and King (2013).)”