In discussion with a friend, Colgate found that neutrinos can develop degeneracy pressure.

It is now easy to determine the degeneracy pressure due to electrons.

White dwarf stars are supported by the degeneracy pressure of the electron gas in their interior.

This increases the pressure of the fermion gas termed degeneracy pressure.

This degeneracy pressure is responsible for keeping certain massive stars from collapsing due to gravity.

Other forces such as gravity and fermionic degeneracy pressure also arise from the momentum conservation.

Neutrons are capable of producing an even higher degeneracy pressure, albeit over a shorter range.

This forces the electrons and protons in the remaining core to form neutrons, which have their own degeneracy pressure.

Only when a star is sufficiently massive to overcome the degeneracy pressure can it collapse into a singularity.

This degeneracy pressure is finally sufficient to stop further collapse of the most central material.