Eddington Model

The Eddington Model is a theoretical framework in astrophysics that describes how stars maintain their stability through a balance between gravity pulling inward and pressure outward. It posits that stars are in a state of thermal equilibrium, where energy produced in the core slowly moves outward to the surface and radiates away. The model uses principles of physics to explain the star’s structure, including temperature, density, and pressure distribution, emphasizing the importance of radiation pressure and thermodynamics. Essentially, it helps scientists understand how stars stay stable over long periods despite ongoing nuclear reactions in their cores.