The Stefan-Boltzmann Law is a fundamental principle in thermodynamics which describes the power radiated from a black body in terms of its temperature. Specifically, it establishes that the total energy radiated per unit surface area of a black body across all wavelengths per unit time (also known as the black-body irradiance or emissive power) is directly proportional to the fourth power of the black body's temperature.
The law is mathematically represented by the equation: \[ Q = e \cdot s \cdot A \cdot (T_{surface}^4 - T_{room}^4) \] where:\
- \( Q \) is the total heat loss due to radiation,
- \( e \) is the emissivity of the material (a dimensionless coefficient),
- \( s \) is the Stefan-Boltzmann constant (\( 5.67 \times 10^{-8} \mathrm{~W/m^2K^4} \)),
- \( A \) is the surface area of the radiating body,
- \( T_{surface} \) is the surface temperature in Kelvin,
- \( T_{room} \) is the ambient temperature around the object, also in Kelvin.
The Stefan-Boltzmann Law helps us understand that objects at a higher temperature emit more thermal radiation compared to objects at a lower temperature.