Oppenheimer–Volkoff limit

E59370

astrophysical concept neutron star property theoretical limit

The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.

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All labels observed (3)

Label	Occurrences
Oppenheimer–Volkoff limit canonical	5
Tolman–Oppenheimer–Volkoff limit	4
Tolman–Oppenheimer–Volkoff limit in relativistic stellar structure	1

How this entity was disambiguated

This entity first appeared as the object of triple T476658 — resolving that mention is where its identity was fixed. The disambiguator weighed these candidate entities and picked the highlighted one (or “None”, minting a new entity). This is how homonymy is resolved: the same surface form can point to different entities.

NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07

Target entity: Oppenheimer–Volkoff limit
Context triple: [Chandrasekhar limit, contrastsWith, Oppenheimer–Volkoff limit]

A. Chandrasekhar limit
The Chandrasekhar limit is the maximum mass a white dwarf star can have before collapsing under its own gravity, playing a crucial role in determining its ultimate fate as a neutron star or black hole.
B. Schwarzschild radius
The Schwarzschild radius is the critical distance from the center of a non-rotating, spherically symmetric mass at which its escape velocity equals the speed of light, defining the boundary of a black hole.
C. Chandrasekhar–Friedman–Schutz instability
The Chandrasekhar–Friedman–Schutz instability is a gravitational-radiation-driven instability in rotating stars that can cause certain oscillation modes to grow by emitting gravitational waves.
D. Oppenheimer–Snyder model
The Oppenheimer–Snyder model is a pioneering theoretical description of gravitational collapse in general relativity, providing one of the first rigorous treatments of how a massive star can form a black hole.
E. Bardeen black hole model
The Bardeen black hole model is a theoretical proposal of a regular (non-singular) black hole solution in general relativity that avoids the central singularity by coupling gravity to nonlinear electrodynamics.
F. None of above. chosen
G. Unsure - the case is ambiguous/there is not enough information to decide.

NED2 Entity disambiguation (via description) gpt-5-mini-2025-08-07

Target entity: Oppenheimer–Volkoff limit
Target entity description: The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.

A. Chandrasekhar limit
The Chandrasekhar limit is the maximum mass a white dwarf star can have before collapsing under its own gravity, playing a crucial role in determining its ultimate fate as a neutron star or black hole.
B. Schwarzschild radius
The Schwarzschild radius is the critical distance from the center of a non-rotating, spherically symmetric mass at which its escape velocity equals the speed of light, defining the boundary of a black hole.
C. Chandrasekhar–Friedman–Schutz instability
The Chandrasekhar–Friedman–Schutz instability is a gravitational-radiation-driven instability in rotating stars that can cause certain oscillation modes to grow by emitting gravitational waves.
D. Oppenheimer–Snyder model
The Oppenheimer–Snyder model is a pioneering theoretical description of gravitational collapse in general relativity, providing one of the first rigorous treatments of how a massive star can form a black hole.
E. Bardeen black hole model
The Bardeen black hole model is a theoretical proposal of a regular (non-singular) black hole solution in general relativity that avoids the central singularity by coupling gravity to nonlinear electrodynamics.
F. None of above. chosen

Statements (42)

Predicate	Object
instanceOf	astrophysical concept ⓘ neutron star property ⓘ theoretical limit ⓘ
alsoKnownAs	Tolman–Oppenheimer–Volkoff limit ⓘ linked to: Oppenheimer–Volkoff limit
appliesTo	degenerate neutron matter ⓘ neutron star ⓘ
assumes	cold neutron star ⓘ isotropic pressure ⓘ non-rotating neutron star ⓘ spherical symmetry ⓘ
basedOn	Einstein field equations ⓘ Tolman–Oppenheimer–Volkoff equation ⓘ
category	compact star physics ⓘ theoretical astrophysics ⓘ
consequenceOf	general relativistic hydrostatic equilibrium ⓘ
constrains	equation of state of ultra-dense matter ⓘ
dependsOn	equation of state of dense nuclear matter ⓘ
derivedBy	George Volkoff ⓘ J. Robert Oppenheimer ⓘ
derivedInCollaborationWith	Richard C. Tolman ⓘ
describes	maximum mass of a neutron star ⓘ
determines	onset of gravitational collapse of neutron stars ⓘ
distinguishedFrom	Chandrasekhar limit ⓘ
field	astrophysics ⓘ general relativity ⓘ
greaterThan	Chandrasekhar limit for white dwarfs ⓘ linked to: Chandrasekhar limit
historicalPublicationYear	1939 ⓘ
implies	collapse to a black hole above the limit ⓘ no stable neutron star configuration above the limit ⓘ
influencedBy	nuclear interaction models ⓘ relativistic corrections to pressure support ⓘ
measuredIn	solar mass ⓘ
namedAfter	George Volkoff ⓘ J. Robert Oppenheimer ⓘ
relatedTo	Chandrasekhar limit ⓘ Tolman–Oppenheimer–Volkoff equation ⓘ neutron star stability ⓘ
typicalRange	approximately 2 to 3 solar masses ⓘ
typicalValue	about 2 solar masses ⓘ
upperBoundOn	gravitational mass of a neutron star ⓘ
usedIn	compact object classification ⓘ interpretation of neutron star observations ⓘ

How these facts were elicited