Search results
Results from the WOW.Com Content Network
Blacksmiths work iron when it is hot enough to emit plainly visible thermal radiation. The color of a star is determined by its temperature, according to Wien's law. In the constellation of Orion, one can compare Betelgeuse (T ≈ 3800 K, upper left), Rigel (T = 12100 K, bottom right), Bellatrix (T = 22000 K, upper right), and Mintaka (T = 31800 K, rightmost of the 3 "belt stars" in the middle).
Comparison of Wien’s curve and the Planck curve. 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.
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
Wilhelm Carl Werner Otto Fritz Franz Wien (German: [ˈvɪlhɛlm ˈviːn] ⓘ; 13 January 1864 – 30 August 1928) was a German physicist who, in 1893, used theories about heat and electromagnetism to deduce Wien's displacement law, which calculates the emission of a blackbody at any temperature from the emission at any one reference temperature.
Retrieved from "https://en.wikipedia.org/w/index.php?title=Wien_displacement_law&oldid=69282641"
Formulas for the various peak wavelengths and mean photon energy were taken from the Wikipedia Wien's displacement law page. The median and quartiles were computed by numerically integrating Planck's law ; however, for any who wish to avoid this, information on percentiles is given in the Planck's law article.
Susning.nu: a Swedish online wiki started in 2001; anyone-can-edit encyclopedia until 2004; shut down in 2009; Svensk uppslagsbok (2 editions, 31 and 32 volumes, 1929–1955) Svenska uppslagsverk: [15] a comprehensive bibliography maintained by collector Christofer Psilander; Swedish Wikipedia (Svenskspråkiga Wikipedia)
Deriving the Stefan–Boltzmann Law using Planck's law. The law can be derived by considering a small flat black body surface radiating out into a half-sphere. This derivation uses spherical coordinates , with θ as the zenith angle and φ as the azimuthal angle; and the small flat blackbody surface lies on the xy-plane, where θ = π / 2 .