Eddington Luminosity

ATRONOMY – TELLAR PHYIC (48) CALCULATOR Eddington Luminosity A precise tool.
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What is the Eddington Luminosity & How does it work?
The Eddington luminosity defines the maximum radiant power a star can emit while remaining in hydrostatic equilibrium. At this limit, the outward pressure of photons balances the inward pull of gravity, preventing further accretion of material onto the stellar surface. Deriving the limit involves equating the radiative force per unit mass, which depends on the opacity (kappa) and the flux, to the gravitational acceleration. The result is a simple linear relationship between the luminosity and the stellar mass, making it a powerful tool for estimating the brightness of massive stars and accreting compact objects. In practice, the Eddington luminosity is often expressed in terms of solar units. For a star of mass (M) measured in solar masses, the luminosity is roughly (1.26times10^{38},M)β€―ergβ€―s⁻¹, or about (3.3times10^{4},M)β€―L(_odot). Exceeding this limit can drive powerful winds and outflows, shaping the evolution of the star and its surrounding environment.
L_{\mathrm{Edd}} = \frac{4\pi G M c}{\kappa}
L_{\mathrm{Edd}} = Eddington luminosity, M = stellar mass, \kappa = opacity (β‰ˆ0.34β€―cmΒ²β€―g⁻¹ for electron scattering), G = gravitational constant, c = speed of light
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Parameters
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Frequently Asked Questions
What is the Eddington luminosity?
The Eddington luminosity is the maximum luminosity a star can achieve without its radiation pressure overcoming gravity, leading to further accretion.
How do you calculate the Eddington luminosity?
It’s calculated using the formula L_Edd = 4Ο€GM / ΞΊ, where G is the gravitational constant, M is the mass of the star, and ΞΊ is the opacity of the stellar material.
What factors determine the Eddington luminosity?
The Eddington luminosity depends on the star’s mass (M), the gravitational constant (G), and the opacity (ΞΊ) of the star’s material.
Can a star exceed its Eddington luminosity?
No, a star cannot exceed its Eddington luminosity without losing mass or undergoing significant changes in its structure.
What happens to a star when it reaches the Eddington limit?
At the Eddington limit, the outward pressure from radiation balances the inward pull of gravity, preventing further accretion onto the star’s surface.

Results are for informational purposes only and do not constitute professional advice.