What is the difference between electron and neutron degeneracy pressure?

Neutron degeneracy pressure, which is a stellar application of the Pauli Exclusion Principle, is actually "stronger" than electron degeneracy pressure, which is also a stellar application of the aforementioned principle because neutrons are more massive and have shorter wavelengths and more closely space energy levels than electrons.

Fundamentally, they are the same principle, but there is a 1/mass term in the spacing of the energy levels that causes neutron degeneracy allow for much closer packing than electron degeneracy. No two electrons can occupy identical states, even under the pressure of a collapsing star of several solar masses. If a star is less than 1.44 solar masses (the Chandrasekhar limit), electron degeneracy will be strong enough to oppose the forces of gravity, and the star will become a white dwarf.

If the star is more massive than 1.44 solar masses, electron degeneracy will eventually crash and neutron degeneracy will be supporting the stellar body, creating a neutron star. If the star is massive enough, even neutron pressure can break down. This is what occurs when black holes are formed. For neutron pressure to break down masses must be larger than about twice or three times that of the sun.

A lot of people are confused with electron and neutron degeneracy pressure. This signifies the manifestation of this phenomenon. This means that there may be neutrons or electrons that are occupying the same space in simultaneous ways.

For example, one type of electron will reach a certain spot while another electron moves to a certain spot. This will go on this way while the electrons or neutrons are in a certain quantum state.

The pressure is important because it makes sure that the star will still have enough energy or fuel to go on. Stars that do not experience this anymore may die after some time.