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The Stefan–Boltzmann constant, σ, is derived from other known physical constants: = where k is the Boltzmann constant, the h is the Planck constant, and c is the speed of light in vacuum. [19] [4]: 388
Boltzmann constant: The Boltzmann constant, k, is one of seven fixed constants defining the International System of Units, the SI, with k = 1.380 649 x 10 −23 J K −1. The Boltzmann constant is a proportionality constant between the quantities temperature (with unit kelvin) and energy (with unit joule).
These include the Boltzmann constant, which gives the correspondence of the dimension temperature to the dimension of energy per degree of freedom, and the Avogadro constant, which gives the correspondence of the dimension of amount of substance with the dimension of count of entities (the latter formally regarded in the SI as being dimensionless).
The law was formulated by Josef Stefan in 1879 and later derived by Ludwig Boltzmann. The formula E = σT 4 is given, where E is the radiant heat emitted from a unit of area per unit time, T is the absolute temperature, and σ = 5.670 367 × 10 −8 W·m −2 ⋅K −4 is the Stefan–Boltzmann constant. [28]
Thus, from the Stefan–Boltzmann law, the luminosity is related to the surface temperature T S, and through it to the color of the star, by = where σ B is Stefan–Boltzmann constant, 5.67 × 10 −8 W m −2 K −4. The luminosity is equal to the total energy produced by the star per unit time.
Balmer's constant: Josef Stefan: 1835–1893 Slovene/Austrian: Stefan's constant [2] Ludwig Boltzmann: 1844–1906 Austrian Boltzmann constant: Henri Victor Regnault: 1810-1878 French Regnault constant: Johannes Rydberg: 1854–1919 Swedish: Rydberg constant: J. J. Thomson: 1856–1940 British Thomson cross section: Erwin Madelung: 1881–1972 ...
The two radiosity components of an opaque surface. The radiosity of an opaque, gray and diffuse surface is given by = +, = + (), where ε is the emissivity of that surface;; σ is the Stefan–Boltzmann constant;
σ is the Stefan-Boltzmann constant. As a result: F i n = ϵ σ T e q 4 {\displaystyle F_{in}=\epsilon \sigma T_{eq}^{4}} is absorbed by the skin layer, while F t h r u = ( 1 − ϵ ) σ T e q 4 {\displaystyle F_{thru}=(1-\epsilon )\sigma T_{eq}^{4}} passes through the skin layer, radiating directly into space.