Stefan-Boltzmann Law
Stefan-Boltzmann law describes the power radiated from a black body, an ideal black surface that absorbs all radiant energy falling on it, in terms of temperature.
Stefan-Boltzmann Law formula
\(\large{ P = \epsilon \; \sigma \; A \; T^4 }\) |
Where:
Units | English | Metric |
\(\large{ P }\) = radiated energy | \(\large{lbf-ft}\) | \(\large{J}\) |
\(\large{ T }\) = absolute temperature of the object emitting | \(\large{R}\) | \(\large{K}\) |
\(\large{ \epsilon }\) (Greek symbol epsilon) = emissivity of the material | \(\large{R}\) | \(\large{K}\) |
\(\large{ A }\) = radiating area | \(\large{ft^2}\) | \(\large{m^2}\) |
\(\large{ \sigma }\) (Greek symbol sigma) = Stefan-Boltzmann constant | \(\large{\frac{Btu}{hr-ft^2-R^4}}\) | \(\large{\frac{W}{m^2-K^4}}\) |
Tags: Equations for Temperature Equations for Energy Equations for Electrical