



Radiance: Integrating the Planck Equation (click on equations to view enlarged)
Above we considered three different spectral units: frequency, ν, (Hz), wavelength, λ, (μm) and wavenumber, σ, (cm^{1}). We derived expressions for the spectral radiances L_{ν}_{ }, L_{λ }, and L_{σ }. To find the radiance, L (W m^{2} sr^{1}), we can integrate any of these over the respective spectral variable. That is,
We will perform the integration of L_{ν} over all frequencies, ν :
. (19)
(Here we used the result Σ n^{4} = ζ (4) = π ^{4}/90, where ζ is the Reimann zeta function) The total radiated power per unit area, called the radiant emittance or radiant exitance, M, can be found by further integrating with respect to solid angle over the hemisphere into which the surface radiates. A source whose radiance is independent of angle is called Lambertian (from Lambert’s cosine law of reflection). This is implicitly assumed for an ideal blackbody, and is a good approximation for many real sources. For a Lambertian source, M is related to L by
so . (20)
This is the StefanBoltzmann law, and the quantity in parentheses is the StefanBoltzmann constant. A common mistake in deriving this result is to assume the factor is 2π rather than π, because there are 2π steradians in the hemisphere, but this neglects the cosθ reduction from Lambert’s cosine law.
Similarly, the total photon radiance is found by integrating L_{σ}^{P} over all frequencies:
(21)
Recall ζ is the Riemann zeta function. ζ(3) ≈ 1.202056903159594 is also known as Apéry’s constant. Integrating L_{σ}^{P} over the hemisphere (again assuming a Lambertian source) gives
(22)
This is the Stefan Boltzmann law for photon radiant emittance. Notice that the total photon flux is proportional to T^{ }^{3}, whereas the total power, given by (5), is proportional to T^{ 4}.

Gascell Simulator 