the Stefan–Boltzmann law

The Stefan–Boltzmann law states that the total energy emitted by a hot object per unit area is proportional to the fourth power of its temperature. In simple terms, the hotter an object is, the more energy it radiates. For example, a glowing piece of metal emits more heat than a cooler piece, because its temperature is higher. This relationship helps us understand phenomena like how the Sun radiates energy into space or how planets emit heat. It’s a fundamental principle connecting temperature and energy emission as a precise mathematical rule.