Chandrasekhar Condition

The Chandrasekhar Condition relates to the stability of white dwarf stars, which are dense remnants of stars like our Sun. It states that there is a maximum mass—about 1.44 times the Sun’s mass—beyond which a white dwarf cannot support itself against gravity using electron degeneracy pressure alone. If its mass exceeds this limit, it will continue to collapse, leading to further transformations like a neutron star or black hole. This condition helps astrophysicists understand why white dwarfs have an upper mass limit and how stars evolve at the end of their life cycle.