The point at which a star's gravitational pressure equals its radiation pressure is known as the Edd
The point at which a star's gravitational pressure equals its radiation pressure is known as the Eddington limit for this quantity. This quantity is equal to four pi times R squared times temperature to the fourth power times the Stefan-Boltzmann constant. A relationship between the period of a star and this quantity is demonstrated in Cepheid variables. This quantity is plotted against temperature on the Hertzsprung-Russell diagram. For 10 points, name this quantity equal to the energy radiated by a star per unit of time.
The point at which a star's gravitational pressure equals its radiation pressure is known as the Eddington limit for this quantity.
luminosity