Page "Chandrasekhar limit" Paragraph 32

After a supernova explosion, a neutron star may be left behind.

Like white dwarfs these objects are extremely compact and are supported by degeneracy pressure, but a neutron star is so massive and compressed that electrons and protons have combined to form neutrons, and the star is thus supported by neutron degeneracy pressure instead of electron degeneracy pressure.

The limit of neutron degeneracy pressure, analogous to the Chandrasekhar limit, is known as the Tolman – Oppenheimer – Volkoff limit.