The magnetic structure of convection-driven numerical dynamos

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Spherical convective dynamos in the rapidly rotating asymptotic regime (2016, methodology): “ection with NR nodal points, and a lateral spherical harmonic decomposition up to degree and order l max. Type CE cases were integrated using the PARODYJA numerical implementation (Dormy et al. 1998; Aubert et al. 2008) using a second-order ﬁnite dierencing scheme in the radial direction with NR gri”
The Magnetic Field of Planet Earth (2010, background): “This has led to very stimulating results (e.g. Bloxham 2000; Olson and Christensen 2002; Christensen and Olson 2003; Gubbins et al. 2007; Willis et al. 2007; Aubert et al. 2008b; Davies et al. 2008).”
Modelling the palaeo-evolution of the geodynamo (2009, methodology): “…one single convection cell near the inner boundary for C, five cells extending from mid-shell to the outer boundary for T. DMFI visualization (Aubert et al. 2008) reveals that the magnetic field is generated according to the classical macroscopic α2 mechanism (Olson et al. 1999), although…”
Rotating convective turbulence in Earth and planetary cores (2015, background): “that qualitatively resemble non-magnetic rotating convection (e.g., Kageyama and Sato, 1997; Olson et al., 1999; Ishihara and Kida, 2002; Aubert et al., 2008; Soderlund et al., 2012; Sreenivasan et al., 2014).”