Limite Eddington (L_Edd)

The Eddington Limit Calculator is a tool used to estimate the maximum luminosity a star can achieve. The Eddington limit, named after astrophysicist Arthur Eddington, represents the maximum luminosity a star can have without the emitted radiation causing significant mass loss. This limit is calculated based on the star's mass, expressed in solar masses (M_sol).

The Eddington limit is calculated using the formula L_Edd = 1.26e31 * M_sol Watts, where M_sol is the star's mass in solar mass units. This means that for a star with a specific mass, there is a luminosity limit beyond which the star would start to lose mass due to radiation pressure. This concept is crucial for understanding stellar evolution and the formation of massive stars.

The Eddington limit is particularly relevant for massive stars, which have a large amount of nuclear fuel to burn. However, even with a large amount of fuel, these stars are still subject to the Eddington limit. If a star exceeds this limit, it can rapidly lose mass, which can affect its evolution and eventually lead to the formation of a supernova.

Care must be taken when applying the Eddington limit, as it assumes the star is in hydrostatic equilibrium and that radiation is the only factor influencing mass loss. In practice, other factors, such as stellar rotation and the presence of magnetic fields, can also influence mass loss and stellar luminosity.