What is the composition of the matter supporting a White Dwarf remnant, contrasting with a Neutron Star?

Electron degenerate matter

The final state of a collapsed star is determined by the mass available to resist gravity, leading to different forms of support. Stars that are less massive than the progenitors of neutron stars (typically less than about eight solar masses) shed their outer layers, leaving behind a White Dwarf. This remnant is stabilized by electron degeneracy pressure. This pressure arises because the electrons are packed so tightly that the Pauli Exclusion Principle prevents further compression, keeping the structure stable. This contrasts fundamentally with the more massive Neutron Star, where gravity is strong enough to overcome electron resistance, forcing electrons into protons and creating neutrons, which are then supported by the much stronger neutron degeneracy pressure.