Calculate Eddington Luminosity

A eddington limiting luminosity produced by the stellar object can be calculated based on the solar mass and stellar mass.







LE = (1.26*1031) * (M / M☉)


LE = Eddington Limiting Luminosity,

M = Stellar Mass,

M☉ = Solar Mass

The example of something with luminosity is the sun. The Luminosity(L) is a measure of the total amount of energy radiated by a star or other celestial object per second. Luminosity is therefore the power output of a star and star's power output across all wavelengths is called its bolometric luminosity.

Luminosity is measured in Watts or in solar luminosities (L⊙) where 1L⊙ = 3.85 x 1026 Watt.

The Eddington luminosity of the sun is the luminosity of the Sun. The maximum luminosity of a source in hydrostatic equilibrium is the Eddington luminosity. If luminosity exceeds the Eddington limit then the radiation pressure drives an outflow

The Eddington limit is obtained by setting the outward radiation pressure equal to the inward gravitational force. Both the forces decrease by inverse square laws, therefore once equality is reached, the hydrodynamic flow is the same throughout the star.