Luminosity Calculator
Calculate Stellar Luminosity
Calculate the luminosity of stars using the Stefan-Boltzmann law: L = 4πR²σT⁴.
Star Parameters
R☉
In solar radii (R☉)
K
Surface temperature in Kelvin
Stefan-Boltzmann Law
L = 4πR²σT⁴
where: σ = 5.670×10⁻⁸ W⋅m⁻²⋅K⁻⁴
Note
Luminosity depends on both the star's radius and temperature. Temperature has a stronger effect (T⁴).
Star Comparison
Sun:1 L☉
Sirius:25.4 L☉
Vega:40.1 L☉
Arcturus:170 L☉
Rigel:120,000 L☉
Betelgeuse:126,000 L☉
About Luminosity
Luminosity is the total amount of energy emitted by a star per unit time. It depends on both the star's radius and surface temperature.
- Proportional to R²
- Proportional to T⁴
- Measured in solar luminosities (L☉)
Applications
- Stellar classification
- Distance measurements (standard candles)
- Hertzsprung-Russell diagrams
- Stellar evolution studies
- Exoplanet habitability zones
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