Stefan-Boltzmann Law: The Glow of Hot Objects

The Stefan–Boltzmann Law says the hotter an object is, the more energy it radiates.
Radiated energy increases with the fourth power of temperature—small heat changes make big differences.
That’s why a slight rise in a star’s temperature makes it glow much brighter.
The law is written as 𝐸=𝜎𝑇4, where 𝜎 is the Stefan–Boltzmann constant.
It explains why black objects radiate heat most efficiently.
This principle lets scientists estimate a star’s luminosity just from its temperature.
Earth absorbs sunlight and re-radiates energy according to this law, shaping climate balance.
Incandescent bulbs glow because their hot filaments radiate energy as predicted by the law.
Satellites use Stefan–Boltzmann calculations to measure planetary temperatures from space.
From glowing stars to household heaters, this law links heat and light in the universe.