Stefan-Boltzmann constant - Revision history

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	<onlyinclude>The '''Stefan-Boltzmann constant''' is a constant of proportionality, σ = <m> 5.67 \times 10^{-8} \frac{W}{m^2K^4}</m> which gives how much [[power]] is radiated by an object at a given [[temperature]].</onlyinclude><ref>Kenneth Krane. ''Modern Physics'', 3rd ed. Hoboken, NJ, USA: John Wiley & Sons, 2012.</ref> It is a physical constant involved in the calculations regarding [[blackbody radiation]] in the [[Stefan-Boltzmann law]]. The constant defines the [[power]] per unit area emitted by a blackbody as a function of its [[temperature]].<ref>Marc L. Kutner. Astronomy: A Physical Perspective, 2nd ed. New York, USA: Cambridge University Press, 2003</ref>		<onlyinclude>The '''Stefan-Boltzmann constant''' is a constant of proportionality, σ = <math> 5.67 \times 10^{-8} \frac{W}{m^2K^4}</math> which gives how much [[power]] is radiated by an object at a given [[temperature]].</onlyinclude><ref>Kenneth Krane. ''Modern Physics'', 3rd ed. Hoboken, NJ, USA: John Wiley & Sons, 2012.</ref> It is a physical constant involved in the calculations regarding [[blackbody radiation]] in the [[Stefan-Boltzmann law]]. The constant defines the [[power]] per unit area emitted by a blackbody as a function of its [[temperature]].<ref>Marc L. Kutner. Astronomy: A Physical Perspective, 2nd ed. New York, USA: Cambridge University Press, 2003</ref>

	This constant was first calculated in 1879 by physicist Josef Stefan, and later again in 1884 by physicist Ludwig Boltzmann who took a more thermodynamic approach.<ref>Encyclopedia Brittanica. (2015, Mar.7). ''Stefan-Boltzmann Law'' [Online]. Available: http://www.britannica.com/EBchecked/topic/564843/Stefan-Boltzmann-law</ref> The Stefan-Boltzmann constant isn't a fundamental constant but is actually made of other constants (see the derivation from the [[Plank radiation formula]] on [http://hyperphysics.phy-astr.gsu.edu/hbase/thermo/stefan2.html#c1 hyperphysics]), which are used together often enough to be treated as a single constant.		This constant was first calculated in 1879 by physicist Josef Stefan, and later again in 1884 by physicist Ludwig Boltzmann who took a more thermodynamic approach.<ref>Encyclopedia Brittanica. (2015, Mar.7). ''Stefan-Boltzmann Law'' [Online]. Available: http://www.britannica.com/EBchecked/topic/564843/Stefan-Boltzmann-law</ref> The Stefan-Boltzmann constant isn't a fundamental constant but is actually made of other constants (see the derivation from the [[Plank radiation formula]] on [http://hyperphysics.phy-astr.gsu.edu/hbase/thermo/stefan2.html#c1 hyperphysics]), which are used together often enough to be treated as a single constant.

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J.williams at 16:59, 12 August 2015

2015-08-12T16:59:07Z

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[[Category:Done 2015-04-01]]
<onlyinclude>The '''Stefan-Boltzmann constant''' is a constant of proportionality, σ = <m> 5.67 \times 10^{-8} \frac{W}{m^2K^4}</m> which gives how much [[power]] is radiated by an object at a given [[temperature]].</onlyinclude><ref>Kenneth Krane. ''Modern Physics'', 3rd ed. Hoboken, NJ, USA: John Wiley & Sons, 2012.</ref> It is a physical constant involved in the calculations regarding [[blackbody radiation]] in the [[Stefan-Boltzmann law]]. The constant defines the [[power]] per unit area emitted by a blackbody as a function of its [[temperature]].<ref>Marc L. Kutner. Astronomy: A Physical Perspective, 2nd ed. New York, USA: Cambridge University Press, 2003</ref>

This constant was first calculated in 1879 by physicist Josef Stefan, and later again in 1884 by physicist Ludwig Boltzmann who took a more thermodynamic approach.<ref>Encyclopedia Brittanica. (2015, Mar.7). ''Stefan-Boltzmann Law'' [Online]. Available: http://www.britannica.com/EBchecked/topic/564843/Stefan-Boltzmann-law</ref> The Stefan-Boltzmann constant isn't a fundamental constant but is actually made of other constants (see the derivation from the [[Plank radiation formula]] on [http://hyperphysics.phy-astr.gsu.edu/hbase/thermo/stefan2.html#c1 hyperphysics]), which are used together often enough to be treated as a single constant.

==References==
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