Stefan-Boltzmann constant

The Stefan-Boltzmann constant is a fundamental value in physics that relates the energy a blackbody (an idealized perfect emitter) emits as radiation to its temperature. Specifically, it quantifies how much energy per unit area is radiated away from an object at a certain temperature, following the Stefan-Boltzmann law: the total energy emitted increases with the fourth power of the temperature. Its value, approximately 5.67×10⁻⁸ W/m²·K⁴, helps scientists understand and calculate thermal radiation for stars, planets, and other objects, serving as a key parameter in thermal physics and astrophysics.