Stefan–Boltzmannn.
/ˈstɛfanˈbəʊltsmən/ Physics.
Used attributively with reference to a law independently discovered by Stefan and Boltzmann (L. E. Boltzmann 1884, in Ann. der Physik u. Chemie XXII. 291; see also Stefan n.).
a. Stefan–Boltzmann law n. the law which states that the total radiation emitted by a black body is proportional to the fourth power of its absolute temperature.
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Stefan–Boltzmann law1898
Stefan law1898
1898 Sci. Abstr.: Physics & Electr. Engin. 1 391 The Stefan–Boltzmann law is confirmed to within 3 to 8%.
1915 R. A. Houstoun Treat. Light xxv. 448 By considering such a cycle Boltzmann proved that the total radiation from a black body was proportional to the fourth power of its absolute temperature. This law had been stated previously but erroneously by Stefan as holding good for all bodies, and as the amended version was due to Boltzmann, it is very often referred to as the Stefan–Boltzmann law.
1977 I. M. Campbell Energy & Atmosphere i. 13 This is related to T through the Stefan–Boltzmann law: E(T) = σT4 where σ is known as the Stefan– Boltzmann constant and has value 5·672 × 10—8 for T in Kelvin and E(T) in Wm—2.
b. Stefan–Boltzmann constant n. the constant in the Stefan–Boltzmann law, equal to 5·67 × 10−8 J m−2 s−1 K−4·.
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Stefan constant1923
Stefan–Boltzmann constant1954
1954 J. C. Johnson Physical Meteorol. iv. 108 σ =..8·22 × 10−11 langley minute−1. σ is called the Stefan-Boltzmann constant.
1958 E. U. Condon & H. Odishaw Handbk. Physics vi. i. 15/1 The total radiation crossing unit area in unit time in all directions in one hemisphere is usually written σT4, where σ is called the Stefan–Boltzmann constant.
This entry has not yet been fully updated (first published 1986; most recently modified version published online September 2018).
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