Numerical dynamo models of Uranus' and Neptune's magnetic fields

By S. Stanley, J. Bloxham. 2006

149 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/1dc43cbff3a653b8b62828102227f72fbe9d244b

How researchers see this paper

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In Astronomy and Astrophysics

1. Jon Fortney
2. N. Nettelmann
3. Ronald Redmer
4. R. Helled
5. J. Anderson
6. Gerald Schubert
7. M. Podolak
8. U. Christensen

In Atmospheric Science

1. J. Anderson
2. Gerald Schubert
3. Jon Fortney
4. U. Christensen
5. Julien Aubert
6. P. Olson

In Molecular Biology

1. Jon Fortney
2. N. Nettelmann
3. Ronald Redmer
4. Gerald Schubert
5. J. Anderson
6. U. Christensen
7. Julien Aubert
8. Johannes Wicht

Citations in the corpus

• New indication for a dichotomy in the interior structure of Uranus and Neptune from the application of modified shape and rotation data (2012, background): “Magnetic field models of Uranus and Neptune require that 60–70% of the region interior to the ionic water layer, corresponding to 0.42–0.56 Rp (Redmer et al., 2011), is stable to convection (Stanley and Bloxham, 2006).”
• Dynamo Scaling Laws and Applications to the Planets (2010, background): “A thin shell dynamo above a stably stratified conducting core might explain the multipolar nature of the magnetic field (Stanley and Bloxham 2004, 2006), but it could run into the problem of a subcritical magnetic Reynolds number, as mentioned above.”
• INTERIOR MODELS OF URANUS AND NEPTUNE (2010, background): “The magnetic fields of Uranus and Neptune provide additional information about their interiors (Ness et al. 1986, 1989; Stanley & Bloxham 2004, 2006).”