Scaling properties of convection-driven dynamos in rotating spherical shells and application to planetary magnetic fields

By U. Christensen, Julien Aubert. 2006

654 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology, Physiology

View Paper: https://www.semanticscholar.org/paper/2d0a75124444e6427c71fa76142a308022f0a730

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Molecular Biology

In Physiology

Citations in the corpus

Simulations of Dynamo Action in Fully Convective Stars (2007, methodology): “Constructing a local Rol as a function of depth in the simulations here (using the power spectra in §5.2) suggests that our models may be on the cusp of entering into the predominantly dipolar regime identified by Christensen & Aubert (2006).”
Dynamo Scaling Laws and Applications to the Planets (2010, methodology): “Sreenivasan and Jones (2006) showed that dynamo models become less dipolar when inertial forces become stronger relative to the Coriolis force.”
Dipole moment scaling for convection-driven planetary dynamos (2005, methodology): “The usual scaling for dynamo fluid velocity u is the magnetic Reynolds number Rm=ud/λ, however, CA [32] have shown that a Rossby number scaling is more compatible with (8).”
Scaling regimes in spherical shell rotating convection (2016, methodology): “Christensen & Aubert (2006), later complemented by King et al. (2010), conducted a systematic parameter study of the scaling properties of convective dynamo models with rigid boundaries and reported the scaling Nu ∼ Ra6/5E8/5 for E = O(10−5).”
Turbulent geodynamo simulations: a leap towards Earth's core (2017, methodology): “However, the magnetic energy of all three simulations correspond to the trend exhibited by the Christensen and Aubert (2006) dataset, which also displays a scatter by a factor 3 to 10 (not shown).”
Conditions for Earth-like geodynamo models (2010, methodology): “Scaling relations (Aubert et al., 2009; Christensen and Aubert, 2006; Olson and Christensen, 2006) can be used to approximately link Rm to the Rayleigh number and the other control parameters.”
Rotating convective turbulence in Earth and planetary cores (2015, background): “Dynamo action becomes possible above some critical value Rmcrit ¼ Oð10Þ (cf. Christensen and Aubert, 2006; Schaeffer and Cardin, 2006).”
MAGNETIC CYCLES IN A CONVECTIVE DYNAMO SIMULATION OF A YOUNG SOLAR-TYPE STAR (2011, background): “Recent simulations of global convective dynamos have focused on rapidly-rotating Boussinesq systems in deep convective shells, often in the context of planetarydynamos (reviewed by Busse 2000; Roberts & Glatzmaier 2001; Christensen & Aubert 2006).”
Quasi-geostrophic flows responsible for the secular variation of the Earth's magnetic field (2008, background): “There, also, strongly columnar regimes have been observed, associated to dipoledominated external fields of the Earth’s type (Olson et al., 1999; Christensen & Aubert, 2006).”
From solar-like to antisolar differential rotation in cool stars (2013, background): “The typical flow lengthscaleℓ is defined asℓ = πd/l̄u, where l̄u is the mean spherical harmonic degree obtained from the kinetic energy spectrum (e.g.Christensen & Aubert 2006; Schrinner et al. 2012).”
Modelling the palaeo-evolution of the geodynamo (2009, methodology): “Furthermore, the results of Christensen & Tilgner (2004), Christensen & Aubert (2006) and Olson & Christensen (2006) need to be extended to cases where the outer core aspect ratio varies, and where the partitioning between the inner- and outer-boundary originated buoyancies also varies.”
New Models of Jupiter in the Context of Juno and Galileo (2019, background): “…magnetic Reynolds number, i.e. the ratio of magnetic field production to Ohmic dissipation, Rm = vrmsd/η, where vrms, d and η denote respectively the rms flow velocity, the thickness of the shell and the magnetic diffusivity, exceeds a critical value Rm & 50 (Christensen and Aubert, 2006).”