# Stefan–Boltzmann constant

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The Stefan–Boltzmann constant (also Stefan's constant), a physical constant denoted by the Greek letter σ, is the constant of proportionality in the Stefan–Boltzmann law: "the total intensity (physics) radiated over all wavelengths increases as the temperature increases", of a black body which is proportional to the fourth power of the thermodynamic temperature.[1] The theory of thermal radiation lays down the theory of quantum mechanics, by using physics to relate to molecular, atomic and sub-atomic levels. Slovenian physicist Josef Stefan formulated the constant in 1879, and it was later derived in 1884 by Austrian physicist Ludwig Boltzmann.[2] The equation can also be derived from Planck's Law, by integrating over all wavelengths at a given temperature, which will represent a small flat black body box.[3] "The amount of thermal radiation emitted increases rapidly and the principal frequency of the radiation becomes higher with increasing temperatures".[4] The Stefan-Boltzmann constant can be used to measure the amount of heat that is emitted by a blackbody, which absorbs all of the radiant energy that hits it, and will emit all the radiant energy. Furthermore, the Stefan–Boltzmann constant allows for temperature (K) to be converted to units for intensity (W/m2), which is power per unit area.

The value of the Stefan–Boltzmann constant is given in SI units by

Template:Physconst

In cgs units the Stefan–Boltzmann constant is:

${\displaystyle \sigma \approx 5.6704\times 10^{-5}\ {\textrm {erg}}\,{\textrm {cm}}^{-2}\,{\textrm {s}}^{-1}\,{\textrm {K}}^{-4}.}$
${\displaystyle \sigma \approx 11.7\times 10^{-8}\ {\textrm {cal}}\,{\textrm {cm}}^{-2}\,{\textrm {day}}^{-1}\,{\textrm {K}}^{-4}.}$

In US customary units the Stefan–Boltzmann constant is:[5]

${\displaystyle \sigma =0.1714\times 10^{-8}\ {\textrm {BTU}}\,{\textrm {hr}}^{-1}\,{\textrm {ft}}^{-2}\,{\textrm {R}}^{-4}.}$

The value of the Stefan–Boltzmann constant is derivable as well as experimentally determinable; see Stefan–Boltzmann law for details. It can be defined in terms of the Boltzmann constant as:

${\displaystyle \sigma ={\frac {2\pi ^{5}k_{\rm {B}}^{4}}{15h^{3}c^{2}}}={\frac {\pi ^{2}k_{\rm {B}}^{4}}{60\hbar ^{3}c^{2}}}=5.670373(21)\,\cdot 10^{-8}\ {\textrm {J}}\,{\textrm {m}}^{-2}\,{\textrm {s}}^{-1}\,{\textrm {K}}^{-4}}$

where:

The CODATA recommended value is calculated from the measured value of the gas constant:

${\displaystyle \sigma ={\frac {2\pi ^{5}R^{4}}{15h^{3}c^{2}N_{\rm {A}}^{4}}}={\frac {32\pi ^{5}hR^{4}R_{\infty }^{4}}{15A_{\rm {r}}({\rm {e}})^{4}M_{\rm {u}}^{4}c^{6}\alpha ^{8}}}}$

where:

.. Dimensional formula : [ M 1 L 0 T -3 K -4]

A related constant is the radiation constant (or radiation density constant) a which is given by:[6]

${\displaystyle a={\frac {4\sigma }{c}}=7.5657\times 10^{-15}{\textrm {erg}}\,{\textrm {cm}}^{-3}\,{\textrm {K}}^{-4}=7.5657\times 10^{-16}{\textrm {J}}\,{\textrm {m}}^{-3}\,{\textrm {K}}^{-4}.}$

## References

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5. Heat and Mass Transfer: a Practical Approach, 3rd Ed. Yunus A. Çengel, McGraw Hill, 2007
6. Radiation constant from ScienceWorld