What are the different laws of Radiation? Explain Stefan Boltzmann’slaw

There are three main laws of radiation: Planck's Law, Stefan-Boltzmann Law, and Wien's Displacement Law.

1. Planck's Law: This law describes the spectral density of electromagnetic radiation emitted by a black body in thermal equilibrium at a given temperature.

2. Wien's Displacement Law: This law states that the black body radiation curve for different temperatures peaks at a wavelength inversely proportional to the temperature.

3. Stefan-Boltzmann Law: This law states that the total energy radiated per unit surface area of a black body is directly proportional to the fourth power of its absolute temperature.

Now, let's explain Stefan-Boltzmann Law in detail:

The Stefan-Boltzmann Law is a principle in physics that says the total energy radiated per unit surface area of a black body (an idealized physical body that absorbs all incident electromagnetic radiation) in thermal equilibrium is directly proportional to the fourth power of its absolute temperature.

Mathematically, it can be written as:

E = σT^4

Where:

• E is the energy radiated per unit surface area,
• σ is the Stefan-Boltzmann constant, approximately equal to 5.67 x 10^-8 watt per square meter per kelvin to the fourth,
• T is the absolute temperature of the body in Kelvin.

This law explains how much heat energy a body radiates or absorbs, which is crucial in many areas of physics and engineering, including astrophysics, climate science, and the design of thermal systems.