The onset of thermal convection in a rapidly rotating sphere

By Chris A. Jones, A. Soward, A. I. Mussa. Journal of Fluid Mechanics, 2000

219 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Biomedical Engineering, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/d788bd7a10db02a48f7214e15dade65409b0ca7a

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Citations in the corpus

A systematic experimental study of rapidly rotating spherical convection in water and liquid gallium (2001, background): “It is only recently, that (Jones et al., 2000) could solve the problem and propose a fully consistent asymptotic approach.”
RECENT GEODYNAMO SIMULATIONS AND OBSERVATIONS OF THE GEOMAGNETIC FIELD (2002, methodology): “For comparison, the Ra-E relation for the onset of convection in a rotating sphere is shown for different Prandtl numbers (Pr) by the solid and dashed lines [Jones et al., 2000].”
Geodynamo theory and simulations (2000, background): “For Ra5Rac , and also for Ra modestly in excess of Rac , convection takes the form of a ‘‘cartridge belt’’ of two-dimensional cells, often called Taylor cells, regularly spaced round the axis of rotation and drifting in longitude about that axis (Roberts, 1968; Jones et al., 2000).”
Convection–driven geodynamo models (2000, methodology): “Since the asymptotic theory of linear convection in a rapidly rotating sphere (or spherical shell) at small E has now been worked out ( Jones et al. 2000 ), at least in the case of uniform heating, we can apply this theory to see what kind of convection we expect at these extreme parameter values.”
The onset of thermal convection in rotating spherical shells (2004, background): “…9, France (Received 19 November 2002 and in revised form 30 July 2003) The correct asymptotic theory for the linear onset of instability of a Boussinesq fluid rotating rapidly in a self-gravitating sphere containing a uniform distribution of heat sources was given recently by Jones et al. (2000).”
Scaling properties of convection-driven dynamos in rotating spherical shells and application to planetary magnetic fields (2006, background): “The critical Rayleigh number for non-magnetic convection at this Prandtl number is Racrit ∼ 2 E−4/3 ≈ 2 × 1019 (Jones et al. 2000), hence convection in the core would be 5000 times supercritical even in the absence of a magnetic field.”