Wien's law

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Wien's law
Wien's law or Wien law may refer to:Wien approximation, an equation used to describe the short-wavelength (high frequency) spectrum of thermal radiation.Wien's displacement law, an equation that describes the relationship between the temperature of an object and the peak wavelength or frequency of the emitted light.Wien-Planck law, an alternate name for the Planck law, which describes the complete spectrum of thermal radiation.
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Black body
In physics, a black body is an object that absorbs all electromagnetic radiation that falls onto it. No radiation passes through it and none is reflected. It is this lack of both transmission and reflection to which the name refers. These properties make black bodies ideal sources of thermal radiation. That is, the amount and wavelength (color) of electromagnetic radiation they emit is directly related to their temperature. Black bodies below around 700 K (430 °C) produce very little radiation at visible wavelengths and appear black (hence the name). Black bodies above this temperature however, produce radiation at visible wavelengths starting at red, going through orange, yellow, and white before ending up at blue as the temperature increases.
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Wien's displacement law
Wien's displacement law is a law of physics that states that there is an inverse relationship between the wavelength of the peak of the emission of a black body and its temperature. where is the peak wavelength in meters, is the temperature of the blackbody in kelvins (K), andb is a constant of proportionality, called Wien's displacement constant and equals 2.897 768 5(51) × 10–3 m K (2002 CODATA recommended value)The two digits between the parentheses denotes the uncertainty (the standard deviation at 68.27 onfidence level) in the two least significant digits of the mantissa.
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Wien's law
A law of physics which describes the wavelength of peak emission of black body radiation as a function of temperature. For the sun, whose surface temperature is 5800 K, the peak wavelength is about 0.5 µm. The law can be used to infer the temperature of a star from its spectral distribution.



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