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Research Papers: Natural and Mixed Convection

Influence of Optical Parameters on Magnetohydrodynamic Natural Convection in a Horizontal Cylindrical Annulus

[+] Author and Article Information
Wei Wang

School of Energy Science and Engineering,
Central South University,
Changsha 410083, China
e-mail: wangwei_neu_china@hotmail.com

Ben-Wen Li

School of Energy and Power Engineering,
Institute of Thermal Engineering,
Dalian University of Technology,
Dalian 116024, China
e-mails: heatli@dlut.edu.cn; heatli@hotmail.com

Zhang-Mao Hu

School of Energy and Power Engineering,
Changsha University of Science and
Technology,
Changsha 410076, China
e-mail: huzhangmao@163.com

1Corresponding author.

Contributed by the Heat Transfer Division of ASME for publication in the JOURNAL OF HEAT TRANSFER. Manuscript received May 27, 2018; final manuscript received January 9, 2019; published online April 17, 2019. Assoc. Editor: Antonio Barletta.

J. Heat Transfer 141(6), 062502 (Apr 17, 2019) (12 pages) Paper No: HT-18-1344; doi: 10.1115/1.4042811 History: Received May 27, 2018; Revised January 09, 2019

The coupled phenomena of radiative–magnetohyrodynamic (MHD) natural convection in a horizontal cylindrical annulus are numerically investigated. The buoyant flow is driven by the temperature difference between the inner and outer cylinder walls, while a circumferential magnetic field induced by a constant electric current is imposed. The hybrid approach of finite volume and discrete ordinates methods (FV-DOM) is developed to solve the nonlinear integro-differential governing equations in polar coordinate system, and accordingly, the influences of Hartmann number, radiation–convection parameter, and optical properties of fluid and wall on thermal and hydrodynamic behaviors of the “downward flow,” originally occurring without consideration of radiation and magnetic field, are mainly discussed. The results indicate that both the circulating flow and heat transfer are weakened by the magnetic field, but its suppression effect on the latter is rather small. Under the influence of magnetic field, the “downward flow” pattern has not been obtained from zero initial condition even for the case of weak radiation of NR = 0.1. Besides, the variation of radiative heat transfer rate with angular positions diminishes for the fluid with strong scattering or weak absorption.

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References

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Figures

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Fig. 1

Physical model with coordinate system and boundary conditions

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Fig. 2

Comparison of isotherms between the present work (lower) and Kuo et al. [4] (upper) for Pr =0.72, Ra =104 with different NR and τL: (a) NR=0.1, τL=1, (b) NR=1, τL=0.1, (c) NR=1, τL=1

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Fig. 3

Comparison of nondimensional radial heat flux distribution along the radial direction with the results of Dua and Cheng [22]

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Fig. 4

Comparison of streamlines between the present work (lower) and Mozayyeni and Rahimi [23] (upper) for different Hartmann numbers: (a) Ha =20, (b) Ha =50, (c) Ha =100

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Fig. 5

Streamlines (Δψ=1, upper) and isotherms (Δθ=0.05, lower) for NR=1, τL=0.1, ω=0, and εw=1 at different Hartmann numbers: (a) Ha =0, (b) Ha =10, (c) Ha =40, (d) Ha =80

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Fig. 6

Effects of Hartmann number on the distribution of local Nusselt numbers for NR=1, τL=0.1, ω=0, and εw=1

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Fig. 7

Streamlines (Δψ=1, upper) and isotherms (Δθ=0.05, lower) for Ha=10, τL=1, ω=0, and εw=1 at different radiation–convection parameters: (a) NR=0, (b) NR=0.1, (c) NR=1, (d) NR=10

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Fig. 8

Streamlines (Δψ=1, upper) and isotherms (Δθ=0.05, lower) for Ha=10, NR=1, ω=0, and εw=1 at different optical thickness: (a) τL=0.1; (b) τL=1; (c) τL=10

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Fig. 9

Effects of optical thickness on the distribution of local Nusselt numbers for Ha=10, NR=1, ω=0, and εw=1

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Fig. 10

Streamlines (Δψ=1, upper) and isotherms (Δθ=0.05, lower) for Ha=10, NR=1, τL=1, and εw=1 at different scattering albedo: (a) ω=0; (b) ω=0.5; (c) ω=0.9

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Fig. 11

Effects of scattering albedo on the distribution of local Nusselt numbers for Ha =10, NR=1, τL=1, and εw=1

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Fig. 12

Streamlines (Δψ=1, upper) and isotherms (Δθ=0.05, lower) for Ha=10, NR=1, τL=1, and ω=0 at different wall emissivity: (a) εw=0.2; (b) εw=0.6; (c) εw=1

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Fig. 13

Effects of wall emissivity on the distribution of local Nusselt numbers for Ha=10, NR=1, τL=1, and ω=0

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