The equation to find the luminosity of a star is the area of the star times its effective temperature times the Stefan-Boltzmann constant. In mathematical terms, this equation can be notated as L ≈ 4πR2σT4.
In the luminosity equation, the area, A, can be found through the formula 4πR², where R is the radius of the star. The effective temperature is derived from the amount of power a star emits based on its surface area. The Stefan-Boltzmann constant is represented by the Greek symbol sigma. It is based on the proportionality wavelengths, temperature and surface area, and is typically expressed in terms of watts, meters and Kelvin.