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Published in:
2011 | OriginalPaper | Chapter
Numerical simulations of rotating Rayleigh-Bénard convection
Authors : Richard J. A. M. Stevens, Herman J. H. Clercx, Detlef Lohse
Published in: Direct and Large-Eddy Simulation VIII
Publisher: Springer Netherlands
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The Rayleigh-Bénard (RB) system is relevant to astro- and geophysical phenomena, including convection in the ocean, the Earth’s outer core, and the outer layer of the Sun. The dimensionless heat transfer (the Nusselt number
Nu
) in the system depends on the Rayleigh number
Ra
=
βg
Δ
L
3
/(
νκ
) and the Prandtl number
Pr
=
ν
/
κ
. Here,
β
is the thermal expansion coefficient,
g
the gravitational acceleration, Δ the temperature difference between the bottom and top, and
ν
and
κ
the kinematic viscosity and the thermal diffusivity, respectively. The rotation rate
H
is used in the form of the Rossby number
Ro
=(
βg
Δ/
L
)/(2
H
). The key question is: How does the heat transfer depend on rotation and the other two control parameters:
Nu
(
Ra
,
Pr
,
Ro
)? Here we will answer this question by giving a summary of our results presented in (Zhong et al.,
2009
; Stevens et al.,
2009
; Stevens et al.,
2010
).