Stellar Luminosity Calculator
Calculate the luminosity of a star with the Stefan-Boltzmann law.
R☉
K
Result
1,0042 L☉
Luminosity: 1.0042 L☉
Result in all units
Step-by-step solution
L = 4πR²σT⁴
What Is Stellar Luminosity?
Luminosity is the total energy a star emits per unit of time. It depends on the star's radius and surface temperature.
How is it calculated?
How Is It Calculated?
Stefan-Boltzmann law: L = 4π × R² × σ × T⁴
σ = 5.67×10⁻⁸ W/(m²·K⁴).
- Enter the star's radius and surface temperature.
Frequently Asked Questions
How does temperature affect brightness?
Because luminosity increases with the fourth power of temperature, a small rise in temperature greatly increases brightness.