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Chandrasekhar Limit




The theoretical upper limit to the mass of a white dwarf star – a compact object made of electron degenerate matter (a dense form of matter which consists of nuclei immersed in a gas of electrons). The Chandrasekhar Limit, which is named after Subrahmanyan Chandrasekhar, has an approximate value of 1.4 solar masses. Above this mass, degenerate electron pressure is insufficient to prevent gravity from collapsing the star further to become either a neutron star or, if the Oppenheimer-Volkoff Limit is also exceeded, a black hole.


Related entry

   • evolution of stars


Related categories

   • STELLAR ASTROPHYSICS
   • GRAVITATIONAL PHYSICS