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Numerical Heat Transfer, Part A: Applications
An International Journal of Computation and Methodology
Volume 72, 2017 - Issue 12
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Original Articles

Radiation effects on turbulent natural convection in optically thick participating fluids using direct numerical simulation

, &
Pages 904-920 | Received 04 Sep 2017, Accepted 14 Nov 2017, Published online: 27 Dec 2017
 

ABSTRACT

We performed a direct numerical simulation (DNS) of the turbulent natural convection between two parallel plates at a Rayleigh number of Ra = 8.0 × 106, focusing on the turbulent natural convection affected by radiation in an optically thick fluid . When the effects of the radiation were considered, the flow structure and temperature distribution in the channel changed as the optical thickness of the fluid increased. The effects of the radiation on the turbulent natural convection were clearly explained by the turbulence statistics from the DNS results.

Nomenclature

cp=

specific heat at constant pressure,

I=

radiative intensity, W/m2sr

Ib=

blackbody radiative  intensity, W/m2sr

g=

gravitational acceleration, m/s2

G=

incident radiation, W/m2

=

production by buoyancy

Gr=

Grashof number

J=

radiosity, W/m2

k=

thermal conductivity, W/mK

l=

integral scale

L=

computational domain size, m

P=

pressure, N/m2

Pl=

Planck number

Pr=

Prandtl number

Pvθ, Pθθ=

production by the mean-temperature gradient

=

radiative heat flux, W/m2

Ra=

Rayleigh number

Rvθ, Rθθ=

production by radiation

=

frictional Reynolds number

t=

time, s

T=

temperature, K

u, v, w=

velocity fluctuation in x-, y-, and z-directions, m/s

ucom=

horizontal velocity fluctuation

U, V, W=

velocity, m/s

=

frictional velocity, m/s

x, y, z=

streamwise, wall-normal, and spanwise coordinate, m

Greek symbols=
α=

thermal diffusivity, m2/s

β=

volumetric thermal expansion coefficient, K−1

Δ=

channel half width, m

=

wall emissivity

Φ=

two-point correlation coefficient

κ=

absorption coefficient, m−1

ν=

kinematic viscosity, m2/s

θ=

temperature fluctuation, K

Θ=

temperature, K

ρ=

density, g/m3

σ=

Stephan–Boltzmann constant, W/m2K4

τ=

optical thickness

=

velocity time scale and temperature time scale

ω=

scattering albedo

Ω=

solid angle, sr

Subscript and superscript=
c=

cold

h=

hot

rms=

root mean square fluctuation intensity

()*=

nondimensional valuable

(¯)=

average valuable

Nomenclature

cp=

specific heat at constant pressure,

I=

radiative intensity, W/m2sr

Ib=

blackbody radiative  intensity, W/m2sr

g=

gravitational acceleration, m/s2

G=

incident radiation, W/m2

=

production by buoyancy

Gr=

Grashof number

J=

radiosity, W/m2

k=

thermal conductivity, W/mK

l=

integral scale

L=

computational domain size, m

P=

pressure, N/m2

Pl=

Planck number

Pr=

Prandtl number

Pvθ, Pθθ=

production by the mean-temperature gradient

=

radiative heat flux, W/m2

Ra=

Rayleigh number

Rvθ, Rθθ=

production by radiation

=

frictional Reynolds number

t=

time, s

T=

temperature, K

u, v, w=

velocity fluctuation in x-, y-, and z-directions, m/s

ucom=

horizontal velocity fluctuation

U, V, W=

velocity, m/s

=

frictional velocity, m/s

x, y, z=

streamwise, wall-normal, and spanwise coordinate, m

Greek symbols=
α=

thermal diffusivity, m2/s

β=

volumetric thermal expansion coefficient, K−1

Δ=

channel half width, m

=

wall emissivity

Φ=

two-point correlation coefficient

κ=

absorption coefficient, m−1

ν=

kinematic viscosity, m2/s

θ=

temperature fluctuation, K

Θ=

temperature, K

ρ=

density, g/m3

σ=

Stephan–Boltzmann constant, W/m2K4

τ=

optical thickness

=

velocity time scale and temperature time scale

ω=

scattering albedo

Ω=

solid angle, sr

Subscript and superscript=
c=

cold

h=

hot

rms=

root mean square fluctuation intensity

()*=

nondimensional valuable

(¯)=

average valuable

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