Stefan-Boltzmann Law

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If a star was marked with L/Teff in the Method column then its diameter was measured using the Stefan-Boltzmann Law. Stellar diameters are usually approximated using the Stefan–Boltzmann law with the star's luminosity and effective temperature. The Stefan-Boltzmann law describes how the temperature, luminosity, and volume of a star are all related in some way.

To calculate a star's diameter with the Stefan-Boltzmann law you must do the following calculation:

Square root of ${\displaystyle ((5772/T)^{4}*L)}$ where ${\displaystyle T}$ represents the effective temperature in Kelvin (not Celsius) and ${\displaystyle L}$ represents the luminosity in terms greater than the Sun.