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18 – Theory of thermography
Planck's formula, when plotted graphically for various temperatures, produces a
family of curves. Following any particular Planck curve, the spectral emittance is zero
at λ = 0, then increases rapidly to a maximum at a wavelength λ
and after passing
max
it approaches zero again at very long wavelengths. The higher the temperature, the
shorter the wavelength at which maximum occurs.
10327103;a3
18
Figure 18.4 Blackbody spectral radiant emittance according to Planck's law, plotted for various absolute
2
3
temperatures. 1: Spectral radiant emittance (W/cm
× 10
(μm)); 2: Wavelength (μm)
18.3.2
Wien's displacement law
By differentiating Planck's formula with respect to λ, and finding the maximum, we
have:
This is Wien's formula (after Wilhelm Wien, 1864–1928), which expresses mathemati-
cally the common observation that colors vary from red to orange or yellow as the
temperature of a thermal radiator increases. The wavelength of the color is the same
as the wavelength calculated for λ
. A good approximation of the value of λ
for
max
max
a given blackbody temperature is obtained by applying the rule-of-thumb 3 000/T
μm. Thus, a very hot star such as Sirius (11 000 K), emitting bluish-white light, radiates
with the peak of spectral radiant emittance occurring within the invisible ultraviolet
spectrum, at wavelength 0.27 μm.
122
Publ. No. 1558407 Rev. a155 – ENGLISH (EN) – February 6, 2006
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