Purdue ME 606: Radiative Heat Flux (Lecture 12)
Table of Contents
Radiative Heat Flux
Consider a ray in direction
through a plane within a participating medium with normal direction
Remember that
Of typically more interest is the divergence of the heat flux vector:
where the incident radiation,
Note: Gη = cuη G = cu, whereof radiation field.
FIGURE: FLUID ELEMENT IN SURROUNDINGS
Combined with the overall fluid energy equation, we have:
where:
(compressible) flow work
βt = thermal expansion coefficient
μΦt = viscous dissipation
1-D Transport
FIGURE: 1-D BOUNDED DOMAIN
Note: We assume that all quantities are spectral; therefore subscripts λ are implied in all terms.
The optical lengths in directions normal to the interface and along the wave are:
Multiply RTE by
:
where
,
where
and
Note: We normally have a similar equation for radiation originating from the top wall.
Observations
- When τL > > 1, the medium is called optically thick, i.e., the photon mean free path is short relative to L.
- When τL < < 1, the medium is called optically thin, i.e., the photon mean free path is large relative to L.
- When τL = 0, the medium is non-participating.
- If scattering is isotropic, Φ = 1.
- For anisotropic scattering,
- If scattering is isotropic,
- Energy flux integrated along a direction in isotropically scattering medium,
and
From Modest’s text, Equation (9.53):
Summary
We have two simultaneous equations, both integro-differential:
- 1 transport equation for I,
- 1 energy balance,
which involve
,
,
.
We often simplify the problem by assuming either:
- T = constant→Ibη is known
-
radiative equilibrium
Note: Many exponential integrals occur.
These integrals are tabulated. Hint: turn cosines into μ‘s.
Also, boundary conditions can be formulated as:
- heat balances at the walls
- specified Iω or radiosity




