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<record version="4" id="166">
 <title>Stefan-Boltzamann law</title>
 <name>StefanBoltzamannLaw</name>
 <created>2006-05-07 17:40:34</created>
 <modified>2006-05-07 19:44:13</modified>
 <type>Law</type>
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 <modifier id="1" name="bloftin"/>
 <author id="1" name="bloftin"/>
 <classification>
	<category scheme="msc" code="44.40.+a"/>
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 <synonyms>
	<synonym concept="Stefan-Boltzamann law" alias="Stefan's law"/>
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 <content>\subsection{Stefan-Boltzmann law}

The Stefan-Boltzmann law, also known as Stefan's law, states that the total energy radiated per unit surface area of a black body in unit time, P is directly proportional to the fourth power of the black body's thermodynamic temperature T (also called absolute temperature):

$$ P(T) = \epsilon \sigma T^{4} $$

The irradiance P has dimensions of power density (energy per time per square distance), and the SI units of measure are joules per second per square meter, or equivalently, watts per square meter. The SI unit for absolute temperature T is the kelvin. e is the emissivity of the blackbody; if it is a perfect blackbody e = 1.

The constant of proportionality $\sigma$, called the Stefan-Boltzmann constant or Stefan's constant, is non-fundamental in the sense that it derives from other known constants of nature. The value of the constant is

$$    \sigma=\frac{2\pi^5 k^4}{15c^2h^3}= 5.670 400 \times 10^{-8} \,\, [\textrm{W\,s}^{-1}\textrm{m}^{-2}\textrm{K}^{-4}].$$

Thus at 100 K the energy flux density is 5.67 W/m2, at 1000 K 56.7 kW/m2, etc.

The law was discovered experimentally by Jožef Stefan (1835-1893) in 1879 and derived theoretically, using thermodynamics, by Ludwig Boltzmann (1844-1906) in 1884. Boltzmann treated a certain ideal heat engine with the light as a working matter instead of the gas. This law is the only physical law of nature named after a Slovene physicist. The law is valid only for ideal black objects, the perfect radiators, called black bodies. Stefan published this law on March 20 in the article Über die Beziehung zwischen der Wärmestrahlung und der Temperatur (On the relationship between thermal radiation and temperature) in the Bulletins from the sessions of the Vienna Academy of Sciences.

\subsection{Derivation}
The Stefan-Boltzmann law can be derived by integrating over all wavelengths the spectral intensity of a black body as given by Planck's radiation law.

$$ P(T)=\int_0^\infty  I(\lambda,T) d\lambda$$

where $I(\lambda,T)$ is the amount of energy emitted by a black body at temperature T per unit surface per unit time per unit solid angle.  The equation for $I$ comes From Planck's radiation law and is given as

$$ I(\lambda,T) = \frac{2 \pi c^2 h}{\lambda^5} \, \frac{1}{e^{hc/ \lambda kT} - 1} $$

which leaves us to integrate

$$ P(T)= 2 \pi c^2 h \int_0^\infty \, \frac{d\lambda}{\lambda^5(e^{hc/ \lambda kT} - 1)} $$

using u substitution by setting 

$$u = \frac{hc}{\lambda kT} $$

so that

$$ du = -\frac{hc}{\lambda^2 kT} d\lambda $$
$$ d\lambda = -\frac{\lambda^2 kT}{hc}$$

substituting this intro the integral yields

$$ P(T)= -2 \pi c^2 h \int_0^\infty \, \frac{\lambda^2 kT du}{\lambda^5 hc(e^{u} - 1)} $$

simplifying a little

$$ P(T)= -2 \pi c kT \int_0^\infty \, \frac{du}{\lambda^3(e^{u} - 1)} du $$

making sure we convert all $\lambda's$ to u's, use

$$ \lambda^3 = (\frac{hc}{u kT})^3 $$

leaving us with

$$ P(T)= -2 \pi c kT (\frac{kT}{hc})^3 \int_0^\infty \, \frac{u^3 du}{(e^{u} - 1)} du $$

\subsection{References}

[1] \PMlinkexternal{National Institute of Standards and Technology}{http://physics.nist.gov/cuu/index.html}

[2] Krane, K., "Modern Physics." Second Edition. New York, John Wiley \&amp; Sons, 1996.

This entry is a derivative of the Stefan-Boltzmann law article from \PMlinkexternal{Wikipedia, the Free Encyclopedia}{http://en.wikipedia.org/wiki/Stefan-Boltzmann_law}. Authors of the orginial article include: Yurivict, Patrick, XJamRastafire , Metacomet and Icairns. History page of the original is \PMlinkexternal{here}{http://en.wikipedia.org/w/index.php?title=Stefan-Boltzmann_law&amp;action=history}</content>
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