Chandrasekhar's equations

Chandrasekhar's equations describe the balance of pressure and gravity in a star, particularly those similar to our Sun. They help determine the maximum mass a white dwarf star can have, known as the Chandrasekhar limit, which is about 1.4 times the mass of the Sun. Beyond this limit, the star can't support itself against gravitational collapse, leading to phenomena like supernovae. Chandrasekhar's work is crucial for understanding stellar evolution and the life cycles of stars, illustrating how mass influences a star's fate in the universe.