The Chandrasekhar limit is a fundamental concept in astrophysics that defines the maximum mass of a stable white dwarf star. This limit is approximately 1.4 times the mass of the Sun. If a white dwarf exceeds this mass, it can no longer support itself against gravitational collapse, leading to a supernova explosion or the formation of a neutron star. Named after the Indian astrophysicist Subrahmanyan Chandrasekhar, who proposed the limit in the 1930s, this concept is crucial for understanding the life cycle of stars. It helps explain the fate of stars after they exhaust their nuclear fuel and provides insights into the formation of various celestial objects.