Planck’s Law for Black Body Radiation
Planck’s Law or Planck’s Radiation Law states the relationship between temperature and radiation emitted by the black body and is given as follows:
[Tex]\bold{B(\nu, T) = \left(\dfrac{2h\nu^3}{c^2}\right) \left(\frac{1}{e^{\frac{h\nu}{k_bT}} – 1}\right)} [/Tex]
Where,
- B(ν, T) is the energy radiated per unit area per unit time form the body,
- ν is Frequency,
- kb is Boltzmann Constant,
- h is Planck’s Constant, and
- c is speed of light in vacuum.
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