Zonal flow driven by strongly supercritical convection in rotating spherical shells

By U. Christensen. Journal of Fluid Mechanics, 2002

227 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Environmental Chemistry, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/07437e3476fe0bff805f876795dc8b72c9f87d25

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Citations in the corpus

From solar-like to antisolar differential rotation in cool stars (2013, background): “Due to the curvature of the spherical shell, the convective columns are slightly tilted in the prograde direction and give rise to Reynolds stresses (a statistical correlation between the convective flow components, seeBusse 1983; Christensen 2002).”
Rotating convective turbulence in Earth and planetary cores (2015, background): “This parame- ter is the square root of Christensen (2002)’s modified Rayleigh number, RoC ’ ffiffiffiffiffiffiffi Ra p .”
The deep wind structure of the giant planets: Results from an anelastic general circulation model (2009, methodology): “Sun et al. (1993), Zhang and Schubert (1996), Aurnou and Olson (2001) and Christensen (2002) show numerical experiments of uniform density fluids with zonal patterns appearing on the surface.”
Dynamo Scaling Laws and Applications to the Planets (2010, background): “Equation 7 fits the convection velocity found in laboratory experiments (Aubert et al. 2001) and numerical simulations (Christensen 2002) of rapidly rotating convection.”
Scaling properties of convection-driven dynamos in rotating spherical shells and application to planetary magnetic fields (2006, background): “…of the magnetic field and stochastic dipole reversals resembling those seen in the paleomagnetic record (Kageyama et al. 1995; Glatzmaier & Roberts 1995a,b; Kuang & Bloxham 1997; Christensen et al. 1998; Busse et al. 1998; Christensen et al. 1999; Kuang & Bloxham 1999; Takahashi et al. 2005).”
Steady zonal flows in spherical shell dynamos (2005, methodology): “In the stress-free case, Christensen (2002) found Uϕ ∝ (Ra∗q)0.4, with no apparent dependence on the Ekman number but with a saturation level at high values of Ra∗q due to a loss of correlation in the small scales of the convection flow.”
Scaling regimes in spherical shell rotating convection (2016, background): “In rotating spherical shells, the axisymmetric zonal flow can represent a significant fraction of the total kinetic energy (e.g. Christensen 2002; Gastine & Wicht 2012; Yadav et al. 2016).”
Jovian atmospheric dynamics: an update after Galileo and Cassini (2005, background): “On the other hand, none of these simulations produce numerous, nested alternating jets outside the tangent cylinder (Christensen 2002) as the Ekman number is reduced from 10−3 to 10−5.”