The Stefan-Boltzmann Law states that the total energy radiated by a black body per unit surface area is proportional to the fourth power of its absolute temperature. This means that as the temperature increases, the energy emitted increases dramatically. The law is mathematically expressed as E = \sigma T^4 , where E is the energy emitted, T is the temperature in Kelvin, and \sigma is the Stefan-Boltzmann constant. This principle is crucial in fields like astrophysics and thermodynamics, as it helps explain how stars, including our Sun, emit energy. Understanding this law allows scientists to calculate the temperature of celestial bodies based on their emitted radiation, providing insights into their composition and behavior.