What is the Eddington limit?

The

Eddington limit, also called Eddington Hearing, is a point where the luminosity emitted by a star or active galaxy is so extreme that it begins to blow from the outer layers of the object. Physically, it is the greatest clarity that can pass through the gas in hydrostatic balance, which means that greater luminosity destroys balance. Hydrostatic balance is a quality that keeps the star wheel and over time approximately the same size. In the real star, the Eddington limit is likely to reach around 120 solar masses, when the star begins to depict its envelope with intense sun wind. Wolf-Rayet stars are massive stars showing Eddington's limit effects that depict 0.001% of their mass through the solar wind per year.

Nuclear reactions in the stars are often highly dependent on the temperature and pressure in the core. For more massive stars, the core is warmer and denser, causing increased reactions. These reactions create abundant heat and overlap over the limit of EddingtonThe radiant pressure out is the strength of the gravitational contraction. However, there are different models where the Eddington limit is exactly, it differs about the factor of two. We are not sure whether the observed star weight limit ~ 150 solar materials is a real limit, or we have not yet found more massive stars.

It is assumed that in the first years of the universe, about 300 million years after the Big Bang, extremely massive stars containing several hundred solar meats could be formed. This is because these stars had virtually no carbon, nitrogen or oxygen (only hydrogen and helium), substances that the careation of the hydrogen talyze, the increase in the brightness of the star. These early stars still fused hydrogen very quickly and had a life of no more than a million years.