Neutron degeneracy pressure

Neutron degeneracy pressure is the pressure produced when the Pauli exclusion principle forces neutrons into higher momentum states as matter is compressed. It can support a neutron star against gravity.

Pauli exclusion principle: The quantum rule that identical fermions cannot occupy the same quantum state. It prevents neutrons from sharing low-energy states, producing resistance to compression.
Neutron star: A compact stellar remnant composed mainly of densely packed neutrons. Its matter is supported partly by neutron degeneracy pressure against gravitational collapse.
Neutron: An electrically neutral subatomic particle found in atomic nuclei and dense stellar matter. Neutron degeneracy pressure arises from the collective state occupation of these particles.
Electron degeneracy pressure: Pressure arising from the exclusion-driven state filling of electrons in dense matter. It supports white dwarfs and differs from neutron pressure in particle mass and stellar regime.
Fermi energy: The highest occupied energy of a fermion system at absolute zero. Compression raises the neutron Fermi energy and the pressure associated with filled states.
Tolman–Oppenheimer–Volkoff limit: The maximum mass of a stable, nonrotating neutron star in general relativity for a given equation of state. It marks where pressure support can no longer balance gravity in a neutron star.
Fermion: A particle with half-integer spin that obeys Fermi–Dirac statistics. Neutrons are fermions, so their available quantum states fill according to exclusion.
Thermal pressure: Pressure produced by the random motion of particles associated with temperature. Unlike thermal pressure, neutron degeneracy pressure persists even at zero temperature.
Fermi gas: A model of many fermions whose state occupation follows Fermi–Dirac statistics. Neutron degeneracy pressure is the pressure of a dense, interacting Fermi system.
Core-collapse supernova: The explosion following the gravitational collapse of a massive star's core. Neutron degeneracy pressure contributes to the rebound and remnant formation during core collapse.

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