Neutron degeneracy pressure is a quantum mechanical phenomenon that arises in neutron stars, preventing them from collapsing under their own gravity by the Pauli exclusion principle, which prohibits neutrons from occupying the same quantum state. This pressure is the primary force counteracting gravitational collapse in neutron stars, maintaining their stability until they reach the Tolman–Oppenheimer–Volkoff limit, beyond which a black hole may form.

Neutron Degeneracy Pressure

Neutron degeneracy pressure

quantum mechanical phenomenon

Neutron stars are the remnants of massive stars that have undergone supernova explosions, resulting in an incredibly dense object primarily composed of neutrons. They exhibit extreme gravitational and magnetic fields, and their study provides insights into fundamental physics and the behavior of matter under extreme conditions.

neutron stars

collapsing under their own gravity

The Pauli Exclusion Principle, formulated by Wolfgang Pauli in 1925, states that no two fermions can occupy the same quantum state simultaneously within a quantum system. This principle is fundamental in explaining the structure of atoms and the behavior of electrons in atoms, leading to the diverse properties of matter.

Pauli exclusion principle

prohibits neutrons

same quantum state

primary force counteracting gravitational collapse

Maintaining Stability

Tolman–Oppenheimer–Volkoff limit

A black hole is a region in space where the gravitational pull is so strong that nothing, not even light, can escape from it. Formed from the remnants of massive stars that have collapsed under their own gravity, black holes challenge our understanding of physics, particularly in the realms of general relativity and quantum mechanics.

Your Courses

Relevant Degrees

Your Lessons