The Chandrasekhar Limit is a theoretical upper bound on the mass of a stable white dwarf star. This limit, approximately 1.4 times the mass of the Sun, was first calculated by Indian astrophysicist Subrahmanyan Chandrasekhar in 1930. Beyond this mass, white dwarfs are unable to support themselves against gravitational collapse due to the electron degeneracy pressure, leading to further gravitational collapse into a neutron star or a black hole.
