Stefan–Boltzmann law

This article does not have any sources. You can help Wikipedia by finding good sources, and adding them. (July 2012)

In quantum physics, the Stefan-Boltzmann law (sometimes called Stefan's Law) states that the black-body radiation energy emitted by a given object is directly proportional to the temperature of the object raised to the fourth power. The equation for this law is:

R=σT⁴

where σ is the Stefan-Boltzmann constant, which is equal to 5.670 373(21) x 10^-8 W m^-2 K^-4, and where R is the energy radiated per unit surface area and per unit time. T is temperature, which is measured in Kelvin scale. Although this law is accurate and helpful, it is only usable for the energy radiated by blackbodies.

This short article about physics can be made longer. You can help Wikipedia by adding to it.