The Chandrasekhar limit, approximately 1.4 times the mass of the Sun, is the maximum mass a white dwarf can have while remaining stable. If a white dwarf exceeds this limit, it can no longer support itself against gravity using electron degeneracy pressure, and it will collapse.
This concept was developed by Indian astrophysicist Subrahmanyan Chandrasekhar in the 1930s. It marks a crucial dividing line in stellar evolution:
- If the remnant core of a dying star is below the Chandrasekhar limit, it becomes a white dwarf.
- If the mass exceeds the limit, the core collapses further—leading to a neutron star or even a black hole, depending on its mass.
The Chandrasekhar limit also plays a vital role in Type Ia supernovae, which occur when a white dwarf in a binary system accumulates enough mass from its companion to exceed the limit, triggering a runaway thermonuclear explosion.
This limit helps define the fates of stars and is a cornerstone of stellar astrophysics and supernova theory.