RECENT GEODYNAMO SIMULATIONS AND OBSERVATIONS OF THE GEOMAGNETIC FIELD

By M. Kono, Paul H. Roberts. 2002

235 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology, Oceanography

View Paper: https://www.semanticscholar.org/paper/367d1d6c31d122c04f9a5cd0ddd982b98965ffbf

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

1. U. Christensen
2. Julien Aubert
3. P. Olson
4. G. Hulot
5. B. Weiss
6. J. Gattacceca
7. S. Stanley
8. P. Rochette

In Molecular Biology

1. U. Christensen
2. Julien Aubert
3. G. Hulot
4. P. Olson
5. B. Weiss
6. J. Gattacceca
7. S. Stanley
8. P. Rochette

In Oceanography

1. U. Christensen
2. Julien Aubert
3. G. Hulot
4. P. Olson
5. Johannes Wicht
6. Alexandre Fournier
7. Chris A. Jones
8. T. Gastine

Citations in the corpus

• An efficient, partitioned ensemble algorithm for simulating ensembles of evolutionary MHD flows at low magnetic Reynolds number (2017, unknown): “It has many applications in astrophysics, planetary science, plasma physics and metallurgical industries, such as MHD turbulence in accretion disks [1], geodynamo simulations [22], plasma containment in fusion reactors [30] and magnetic damping of jets and vortices [4].”
• Dipole moment scaling for convection-driven planetary dynamos (2005, background): “Numerical dynamos driven by Boussinesq convection in thick, rotating fluid shells commonly produce magnetic fields similar to the geomagnetic field, with a strong axial dipole component, secular variation, and occasional polarity reversals [11–13].”
• Scaling properties of convection-driven dynamos in rotating spherical shells and application to planetary magnetic fields (2006, methodology): “We note that our definition of the Ekman number is conservative; with the definition of Kono & Roberts (2002), E ′ = ν/(2 r 2o), the range is roughly from 2 × 10−7 to 6 × 10−5.”
• Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation (2010, background): “The motions must be threedimensional and have significantly complex morphologies (for a review of planetary dynamo theory, see Kono and Roberts 2002).”
• Conditions for Earth-like geodynamo models (2010, background): “This paper follows the spirit of the reviews by (Dormy et al. (2000) and Kono and Roberts, 2002), who extensively discussed which properties of the geomagnetic field could be considered wellestablished (at the time of writing) and compared the limited number of geodynamo models then available…”