Explain the Chandrasekhar limit in simple terms.
The Chandrasekhar limit represents a fundamental threshold in astrophysics. Imagine a star that has exhausted its nuclear fuel and has settled into a stable state as a white dwarf. The pressure supporting this star against gravitational collapse is primarily due to the quantum mechanical effect of electron degeneracy. However, as mass increases, the electrons are forced into higher energy states, and relativistic effects become significant. Above approximately 1.4 solar masses, the electron degeneracy pressure is no longer sufficient to counteract gravity. The star must then undergo further collapse, leading to phenomena like a Type Ia supernova or the formation of a neutron star. This is not a matter of opinion but of rigorous derivation.
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