Numerical simulations of rotating Rayleigh-Bénard convection

Richard J.A.M. Stevens; Herman J.H. Clercx; Detlef Lohse

doi:10.1007/978-94-007-2482-2_57

Numerical simulations of rotating Rayleigh-Bénard convection

Richard J.A.M. Stevens, Herman J.H. Clercx, Detlef Lohse

Physics of Fluids

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › Academic › peer-review

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Abstract

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=βgΔL 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=(βgΔ/L)/(2H). 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).

Original language	English
Title of host publication	Direct and Large-Eddy Simulation VIII
Editors	Hans Kuerten, Bernard Geurts, Vincenzo Armenio, Jochen Fröhlich
Place of Publication	Dordrecht
Publisher	Springer
Pages	359-364
Number of pages	6
ISBN (Print)	978-94-007-2481-5
DOIs	https://doi.org/10.1007/978-94-007-2482-2_57
Publication status	Published - 2011
Event	8th ERCOFTAC Workshop on Direct and Large-Eddy Simulation VIII, DLES 2010 - Eindhoven University of Technology, Eindhoven, Netherlands Duration: 7 Jul 2010 → 9 Jul 2010 Conference number: 8

Publication series

Name	ERCOFTAC series
Publisher	Springer
Volume	15
ISSN (Print)	1382-4309

Workshop

Workshop	8th ERCOFTAC Workshop on Direct and Large-Eddy Simulation VIII, DLES 2010
Abbreviated title	DLES
Country/Territory	Netherlands
City	Eindhoven
Period	7/07/10 → 9/07/10

Keywords

Rayleigh number
Direct numerical simulation
Thermal boundary layer
Heat transfer enhancement
Rossby number

Access to Document

10.1007/978-94-007-2482-2_57

Cite this

@inproceedings{92dc85feefdd40888698d260f5413c71,

title = "Numerical simulations of rotating Rayleigh-B{\'e}nard convection",

abstract = "The Rayleigh-B{\'e}nard (RB) system is relevant to astro- and geophysical phenomena, including convection in the ocean, the Earth{\textquoteright}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=βgΔL 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=(βgΔ/L)/(2H). 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).",

keywords = "Rayleigh number, Direct numerical simulation, Thermal boundary layer, Heat transfer enhancement, Rossby number",

author = "Stevens, {Richard J.A.M.} and Clercx, {Herman J.H.} and Detlef Lohse",

year = "2011",

doi = "10.1007/978-94-007-2482-2_57",

language = "English",

isbn = "978-94-007-2481-5",

series = "ERCOFTAC series",

publisher = "Springer",

pages = "359--364",

editor = "Hans Kuerten and Bernard Geurts and Vincenzo Armenio and Jochen Fr{\"o}hlich",

booktitle = "Direct and Large-Eddy Simulation VIII",

address = "Germany",

note = "8th ERCOFTAC Workshop on Direct and Large-Eddy Simulation VIII, DLES 2010, DLES ; Conference date: 07-07-2010 Through 09-07-2010",

}

Stevens, RJAM, Clercx, HJH & Lohse, D 2011, Numerical simulations of rotating Rayleigh-Bénard convection. in H Kuerten, B Geurts, V Armenio & J Fröhlich (eds), Direct and Large-Eddy Simulation VIII. ERCOFTAC series, vol. 15, Springer, Dordrecht, pp. 359-364, 8th ERCOFTAC Workshop on Direct and Large-Eddy Simulation VIII, DLES 2010, Eindhoven, Netherlands, 7/07/10. https://doi.org/10.1007/978-94-007-2482-2_57

Numerical simulations of rotating Rayleigh-Bénard convection. / Stevens, Richard J.A.M.; Clercx, Herman J.H.; Lohse, Detlef.
Direct and Large-Eddy Simulation VIII. ed. / Hans Kuerten; Bernard Geurts; Vincenzo Armenio; Jochen Fröhlich. Dordrecht: Springer, 2011. p. 359-364 (ERCOFTAC series; Vol. 15).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › Academic › peer-review

TY - GEN

T1 - Numerical simulations of rotating Rayleigh-Bénard convection

AU - Stevens, Richard J.A.M.

AU - Clercx, Herman J.H.

AU - Lohse, Detlef

N1 - Conference code: 8

PY - 2011

Y1 - 2011

N2 - 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=βgΔL 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=(βgΔ/L)/(2H). 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).

AB - 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=βgΔL 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=(βgΔ/L)/(2H). 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).

KW - Rayleigh number

KW - Direct numerical simulation

KW - Thermal boundary layer

KW - Heat transfer enhancement

KW - Rossby number

U2 - 10.1007/978-94-007-2482-2_57

DO - 10.1007/978-94-007-2482-2_57

M3 - Conference contribution

SN - 978-94-007-2481-5

T3 - ERCOFTAC series

SP - 359

EP - 364

BT - Direct and Large-Eddy Simulation VIII

A2 - Kuerten, Hans

A2 - Geurts, Bernard

A2 - Armenio, Vincenzo

A2 - Fröhlich, Jochen

PB - Springer

CY - Dordrecht

T2 - 8th ERCOFTAC Workshop on Direct and Large-Eddy Simulation VIII, DLES 2010

Y2 - 7 July 2010 through 9 July 2010

ER -

Numerical simulations of rotating Rayleigh-Bénard convection

Abstract

Publication series

Workshop

Keywords

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