Dipole moment scaling for convection-driven planetary dynamos

By P. Olson, U. Christensen. 2005

269 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology, Oceanography

View Paper: https://www.semanticscholar.org/paper/792cbda2aa7c76dfeb5fe037f4458874953a07fe

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Citations in the corpus

Magnetic energy fluxes in sub-Alfvénic planet star and moon planet interactions (2013, methodology): “(23) of Olson & Christensen (2006), which we scale to values of Jupiter and find Mexo = MJ ( Rexo RJ )10/3 , (59) with the magnetic moment of Jupiter MJ = 1.56 × 1027 Am2 (Connerney et al. 1982) and the equatorial radius of Jupiter RJ = 71 492 km (Lindal et al. 1981).”
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.”
The On/Off Nature of Star-Planet Interactions (2007, background): “…Jupiters are expected to be weaker than Jupiter’s due to probable tidal locking and slower spin rates (Sanchez-Lavega 2004, Griessmeier et al. 2004), Olson & Christensen (2006) calculated that the magnetic field of a planet with even a tenth of Jupiter’s rotation rate would still have a strong…”
Simulations of Dynamo Action in Fully Convective Stars (2007, background): “They and others have suggested that predominantly dipolar fields are realized when inertial forces are small relative to Coriolis forces (see also Sreenivasan & Jones 2006; Olson & Christensen 2006).”
Dynamo Scaling Laws and Applications to the Planets (2010, background): “For the gas planets, and in particular for Uranus and Neptune, Olson and Christensen (2006) estimated values of Ro an order of magnitude smaller than for the Earth’s core.”
Low‐degree structure in Mercury's planetary magnetic field (2012, background): “Multipolar dynamos can produce a weak field [e.g., Olson and Christensen, 2006], but such fields are not dipole dominated.”
Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation (2010, background): “In addition, the scaling law of Olson and Christensen (2006) for Rol is purely empirical and depends on viscosity and thermal diffusivity, whose values in the numerical models on which the scaling has been based are far removed from those in planetary cores.”
The magnetic structure of convection-driven numerical dynamos (2008, background): “As one increases the convective forcing, the onset of reversals is usually close to the point where the dipole part of the generated magnetic field ceases to dominate the magnetic spectrum (Olson & Christensen 2006).”
Conditions for Earth-like geodynamo models (2010, methodology): “…which is equivalent) tends to generate less dipolar fields than are found inmodels that are driven from below (Kutzner and Christensen, 2002; Olson and Christensen, 2006), although the choice of a fixed flux condition instead of a fixed temperature condition at the CMB reduces this trend…”
Sulfur's impact on core evolution and magnetic field generation on Ganymede (2005, background): “[35] Recent numerical dynamo studies provide empirical scaling laws for planetary dynamo magnetic field strength, B, as a function of the dynamo simulation control parameters [Christensen and Aubert, 2006;Olson and Christensen, 2006].”