The Tolman-Oppenheimer-Volkoff limit is the maximum mass that a neutron star can have before collapsing into a black hole due to gravitational forces overwhelming neutron degeneracy pressure. This theoretical limit is crucial in astrophysics for understanding the life cycles of massive stars and the formation of black holes.

Tolman-Oppenheimer-Volkoff Limit

Tolman-Oppenheimer-Volkoff limit

maximum mass

A neutron star is the collapsed core of a massive star which has undergone a supernova explosion, characterized by an incredibly high density where protons and electrons have combined to form neutrons. These stars are incredibly small in size, typically about 20 kilometers in diameter, yet they possess a mass greater than that of the Sun, leading to intense gravitational and magnetic fields.

neutron star

collapsing into a black hole

Gravitational forces are the attractive forces between masses, which govern the motion of celestial bodies and the structure of the universe. They are described by Newton's law of universal gravitation and further refined by Einstein's general theory of relativity, which accounts for the curvature of spacetime around massive objects.

gravitational forces

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

theoretical limit

Astrophysics is the branch of astronomy that employs the principles of physics and chemistry to understand how stars, planets, and galaxies form, evolve, and interact. It seeks to unravel the mysteries of the universe, from the behavior of subatomic particles in extreme environments to the large-scale structure of the cosmos.

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