Equations · equation

Chandrasekhar Limit

Astrophysics · 1931

Equation
M_Ch ∝ (ℏc/G)^(3/2)/(μₑmₚ)² ≈ 1.4 M☉
Field
Astrophysics
Named After
Subrahmanyan Chandrasekhar
Year
1931

Symbols

M_Ch the maximum white-dwarf mass · ℏ reduced Planck constant · c speed of light · G gravitational constant · μₑ electrons per nucleon · mₚ proton mass · M☉ solar mass

Significance

Above about 1.4 solar masses, electron degeneracy pressure can no longer hold a dead star up against its own gravity, and collapse continues to a neutron star or a black hole. Worked out by Chandrasekhar at 19, aboard the ship carrying him to Cambridge, and disputed for a decade by Eddington, who thought the conclusion absurd. It sets the scale for Type Ia supernovae, which is why they can be used as distance markers at all — but the old line that they all detonate at exactly this mass has not survived: they are standardised after the fact, by correcting brightness against how fast the light curve fades, and a good part of them may come from white dwarfs that never reached the limit.

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From the Equations database in Notion, last edited 2026-08-26. This page is the row, rendered by the build; nothing on it is written by hand.