Chandrasekhar Limit Calculator
Chandrasekhar Limit
Calculate the maximum mass of a stable white dwarf star based on composition, and determine whether a remnant will become a white dwarf, neutron star, or black hole.
Formula
Chandrasekhar Limit = 1.44 x (Ye / 0.5)^2 solar masses; White Dwarf: M < Chandrasekhar Limit; Neutron Star: Chandrasekhar Limit < M < ~2.16 solar masses; Black Hole: M > ~2.16 solar masses
Frequently Asked Questions
What is the Chandrasekhar limit?
The Chandrasekhar limit is approximately 1.44 solar masses, the maximum mass a white dwarf can have before electron degeneracy pressure can no longer support it against gravitational collapse.
What happens above the Chandrasekhar limit?
A remnant above the Chandrasekhar limit but below about 2-3 solar masses becomes a neutron star, supported by neutron degeneracy pressure. Above that, it collapses into a black hole.
Why is the electron fraction important?
The electron fraction Ye determines the number of electrons per baryon. The Chandrasekhar limit scales as Ye squared, so composition affects the exact mass threshold.
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