Formula for Stefan-Boltzmann Law
Mathematically, Stefan Boltzmann’s law for the black body is given by
P/A ∝T4
OR
P = σAT4
Where,
- P is the power radiated,
- A is the surface area of the black body,
- T is the temperature of the body and
- σ is the Stefan-Boltzmann constant.
Objects which are not black bodies emit less radiation as they can absorb radiation as well. For such objects, Stefan Boltzmann’s law is as follows:
P/A ∝ eT4
OR
P = σeAT4
Where, e is the emissivity of the object and can have value from 0 to 1.
Stefan-Boltzmann Law
Stefan-Boltzmann Law relates the power radiated by the black body to its temperature and surface area. In the study of thermodynamics and astrophysics, the Stefan-Boltzmann Law is widely used to better our understanding of the subject. Other than this, Stefan-Boltzmann Law helps scientists understand the behavior of objects that emit radiation, such as stars and planets. Stefan-Boltzmann Law also has some applications in the real world as well such as, in designing solar panels and other energy conversion instruments.
Table of Content
- What is Stefan-Boltzmann Law?
- Formula for Stefan-Boltzmann Law
- Stefan-Boltzmann Constant
- Value of Stefan-Boltzmann Constant
- Formula for Stefan-Boltzmann Constant
- Black Body Radiation
- Planck’s Law for Black Body Radiation
- Derivation of Stefan-Boltzmann Constant
- Calculation of Stefan-Boltzmann Constant
- Applications of Stefan-Boltzmann Law
- Sample Problems on Stefan-Boltzmann Law