Overview
The Stefan-Boltzmann Law describes the relationship between the temperature of a black body and the energy it radiates. The equation is:

Where:

• L(T) is the total radiated power (energy per unit area),

• T is the absolute temperature of the body,

• σ is the Stefan-Boltzmann constant.

Significance
The Stefan-Boltzmann Law is vital in astrophysics for studying star radiation, in thermal imaging for detecting heat, and in climate science to model energy transfer and radiation in Earth’s atmosphere.