Name: FLIR T640
Brand: FLIR
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Theory of thermography

Figure 33.5 Wilhelm Wien (1864–1928)

The sun (approx. 6 000 K) emits yellow light, peaking at about 0.5 μm in the middle of

the visible light spectrum.

At room temperature (300 K) the peak of radiant emittance lies at 9.7 μm, in the far infra-

red, while at the temperature of liquid nitrogen (77 K) the maximum of the almost insignif-

icant amount of radiant emittance occurs at 38 μm, in the extreme infrared wavelengths.

Figure 33.6 Planckian curves plotted on semi-log scales from 100 K to 1000 K. The dotted line represents

the locus of maximum radiant emittance at each temperature as described by Wien's displacement law. 1:

Spectral radiant emittance (W/cm

(μm)); 2: Wavelength (μm).

33.3.3 Stefan-Boltzmann's law

By integrating Planck’s formula from λ = 0 to λ = ∞, we obtain the total radiant emittance

) of a blackbody:

This is the Stefan-Boltzmann formula (after Josef Stefan, 1835–1893, and Ludwig Boltz-

mann, 1844–1906), which states that the total emissive power of a blackbody is propor-

tional to the fourth power of its absolute temperature. Graphically, W

represents the

area below the Planck curve for a particular temperature. It can be shown that the radiant

emittance in the interval λ = 0 to λ

max

is only 25% of the total, which represents about the

amount of the sun’s radiation which lies inside the visible light spectrum.

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