Calcolatore Luminosita di Eddington
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Eddington Luminosity
14,708,643,955,456,562,000,000,000,000,000.000 W
Eddington Luminosity vs Object Mass
Formula
## The Eddington Luminosity The maximum luminosity where radiation pressure on infalling matter balances gravitational attraction. ### Formula **L_Edd = 4π G M c / κ** Using electron-scattering opacity κ ≈ 0.034 m²/kg for ionised hydrogen. For a solar-mass object, L_Edd ≈ 3.3 × 10⁴ L_sun. Exceeding L_Edd causes radiation-driven mass loss (stellar winds, super-Eddington outbursts).
Esempio Risolto
A 1-solar-mass object.
- 01L_Edd = 4π G M c / κ
- 02= 4π × 6.674e-11 × 1.989e30 × 2.998e8 / 0.034
- 03Numerator = 4π × 3.979e28 = 4.988e29
- 04L_Edd = 4.988e29 / 0.034 ≈ 1.47e31 W ≈ 38 300 L_sun
Domande Frequenti
Can stars exceed the Eddington limit?
Briefly, yes. Super-Eddington luminosities drive powerful mass outflows. Some very massive stars and accreting objects transiently exceed it.
Why does the Eddington limit matter for black holes?
It sets the maximum accretion rate onto a black hole. Faster accretion would blow away the infalling material.
Does opacity affect the limit?
Yes. Higher opacity lowers L_Edd because radiation couples more effectively to matter. The electron-scattering value is a minimum opacity for ionised gas.