Calculadora de Luminosidade de Stefan-Boltzmann — Formula
## Stefan-Boltzmann Law
The total power radiated by a spherical blackbody:
**L = 4π R² σ T⁴**
- σ = 5.670 × 10⁻⁸ W m⁻² K⁻⁴ (Stefan-Boltzmann constant)
- R = stellar radius
- T = surface (effective) temperature
Luminosity depends on radius squared and temperature to the fourth power.
The total power radiated by a spherical blackbody:
**L = 4π R² σ T⁴**
- σ = 5.670 × 10⁻⁸ W m⁻² K⁻⁴ (Stefan-Boltzmann constant)
- R = stellar radius
- T = surface (effective) temperature
Luminosity depends on radius squared and temperature to the fourth power.
Exemplo Resolvido
The Sun: R = 6.957e8 m, T = 5778 K.
- L = 4π R² σ T⁴
- R² = (6.957e8)² = 4.840e17
- 4π R² = 6.079e18 m²
- T⁴ = 5778⁴ = 1.115e15
- σ T⁴ = 5.670e-8 × 1.115e15 = 6.322e7
- L = 6.079e18 × 6.322e7 ≈ 3.843e26 W ≈ 1.00 L_sun