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Chandrasekhar Limit
The theoretical upper limit to the mass of a white dwarf star – approximately 1.4 solar masses; it is named after Subrahmanyan Chandrasekhar. 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
• stars, evolution
Related categories
• STELLAR ASTROPHYSICS
• GRAVITATIONAL PHYSICS
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