TOV Limit
Version 1.0.0 · Updated 2026-07-28
CORE DEFINITION
In astrophysics, the Tolman–Oppenheimer–Volkoff equation is a constraint equation in the framework of general relativity that describes the structure of a spherically symmetric, isotropic object in hydrostatic equilibrium. It describes the relativistic hydrostatic equilibrium of a star under radiation pressure and its own gravity.
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In astrophysics, the Tolman–Oppenheimer–Volkoff equation is a constraint equation in the framework of general relativity that describes the structure of a spherically symmetric, isotropic object in hydrostatic equilibrium. It describes the relativistic hydrostatic equilibrium of a star under radiation pressure and its own gravity.
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Under general relativity, neutron stars resist gravity via neutron degeneracy pressure. Tolman, Oppenheimer, and Volkov derived their mass limit (about 2-3 solar masses, often cited as ~2.17 M☉). Beyond this limit, degeneracy pressure cannot withstand gravity, and the star irreversibly collapses into a black hole—quantitative change crossing a threshold triggers a phase transition (a jump in the state of matter).
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- zh.wikipedia.orghttps://zh.wikipedia.org/wiki/%E6%89%98%E5%B0%94%E6%9B%BC-%E5%A5%A5%E6%9C%AC%E6%B5%B7%E9%BB%98-%E6%B2%83%E5%B0%94%E7%A7%91%E5%A4%AB%E6%96%B9%E7%A8%8Bverified
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