Final answer:
The σ Stefan-Boltzmann constant is a foundational component of the Stefan-Boltzmann law, used to calculate energy radiated by black bodies in terms of temperature. This constant, approximately 5.67 × 10^-8 W/m²/K^4, allows physicists to estimate a star's energy output using its measured temperature.
Step-by-step explanation:
The σ Stefan-Boltzmann constant is a physical constant that is fundamental to the Stefan-Boltzmann law, which describes the total power radiated per unit surface area of a black body in terms of its temperature.
Specifically, this constant is symbolized as σ and has a numerical value approximately equal to 5.67 × 10-8 W/m²/K4. It is derived from a combination of other constants, including Planck's constant (h), the speed of light (c), and the Boltzmann constant (kB).
The law can be expressed in the formula F = σT4, where F is the total emitted energy per unit area, σ is the Stefan-Boltzmann constant, and T is the absolute temperature in Kelvin. When applied, this law enables scientists to calculate the energy output of a black body, such as a star, by knowing its temperature.