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Concept
Wien approximation
Summary
Wien's approximation (also sometimes called Wien's law or the Wien distribution law) is a law of physics used to describe the spectrum of thermal radiation (frequently called the blackbody function). This law was first derived by Wilhelm Wien in 1896. The equation does accurately describe the short wavelength (high frequency) spectrum of thermal emission from objects, but it fails to accurately fit the experimental data for long wavelengths (low frequency) emission.
Wien derived his law from thermodynamic arguments, several years before Planck introduced the quantization of radiation.
Wien's original paper did not contain the Planck constant. In this paper, Wien took the wavelength of black body radiation and combined it with the Maxwell–Boltzmann energy distribution for atoms. The exponential curve was created by the use of Euler's number e raised to the power of the temperature multiplied by a constant. Fundamental constants were later introduced by Max Planck.
The law may be written as
(note the simple exponential frequency dependence of this approximation) or, by introducing natural Planck units:
where:
is the amount of energy per unit surface area per unit time per unit solid angle per unit frequency emitted at a frequency ν.
is the temperature of the black body.
is the ratio of frequency over temperature.
is the Planck constant.
is the speed of light.
is the Boltzmann constant.
This equation may also be written as
where is the amount of energy per unit surface area per unit time per unit solid angle per unit wavelength emitted at a wavelength λ.
The peak value of this curve, as determined by setting the derivative of the equation equal to zero and solving, occurs at a wavelength λmax and frequency νmax of:
The Wien approximation was originally proposed as a description of the complete spectrum of thermal radiation, although it failed to accurately describe long wavelength (low frequency) emission. However, it was soon superseded by Planck's law which accurately describes the full spectrum, derived by treating the radiation as a photon gas and accordingly applying Bose–Einstein in place of Maxwell-Boltzmann statistics.
Official source
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