black-body radiation law 

The black-body radiation law is a fundamental concept in physics that describes the emission of electromagnetic radiation by an idealized object called a black body. A black body is an object that absorbs all electromagnetic radiation that falls on it, and emits radiation that is solely determined by its temperature.

The black-body radiation law states that the intensity of radiation emitted by a black body is proportional to the fourth power of its temperature, and is given by the formula:

I = σT^4

where I is the intensity of radiation emitted, T is the temperature of the black body, and σ is a constant known as the Stefan-Boltzmann constant. The Stefan-Boltzmann constant has a value of approximately 5.67 × 10^-8 W/m^2K^4.

The black-body radiation law was first derived by the German physicist Max Planck in 1900, and it has since been shown to be a fundamental law of physics that applies to all objects that emit radiation. The law has important applications in fields such as astrophysics, where it is used to study the radiation emitted by stars and other celestial objects.

The black-body radiation law also played a crucial role in the development of quantum mechanics, as it was the starting point for Planck’s derivation of the quantization of energy levels in atoms. The law has continued to be a subject of active research in physics, as scientists seek to better understand the properties of black bodies and their role in the behavior of materials and the universe as a whole. Read More about School Management System.