black hole no-hair theorem
E6813
The black hole no-hair theorem is a principle in general relativity stating that stationary black holes are completely characterized by only a few macroscopic parameters—mass, electric charge, and angular momentum—regardless of the details of the matter that formed them.
All labels observed (3)
| Label | Occurrences |
|---|---|
| no-hair theorem | 3 |
| black hole no-hair theorem canonical | 1 |
| no-hair theorem for black holes | 1 |
How this entity was disambiguated
This entity first appeared as the object of triple T65787 — 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: black hole no-hair theorem Context triple: [Schwarzschild black hole, obeysLaw, black hole no-hair theorem]
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A.
Schwarzschild black hole
A Schwarzschild black hole is the simplest theoretical black hole solution in general relativity, describing a static, spherically symmetric, non-rotating, uncharged mass with an event horizon defined by the Schwarzschild radius.
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B.
Bekenstein–Hawking entropy
Bekenstein–Hawking entropy is the thermodynamic entropy associated with a black hole, proportional to the area of its event horizon and fundamental in linking gravity, quantum theory, and thermodynamics.
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C.
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.
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D.
Einstein field equations
The Einstein field equations are the core mathematical framework of general relativity, relating the curvature of spacetime to the distribution of matter and energy.
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E.
Higgs boson
The Higgs boson is an elementary particle in the Standard Model whose associated field gives mass to other fundamental particles, confirming a key mechanism of particle physics.
- 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: black hole no-hair theorem Target entity description: The black hole no-hair theorem is a principle in general relativity stating that stationary black holes are completely characterized by only a few macroscopic parameters—mass, electric charge, and angular momentum—regardless of the details of the matter that formed them.
-
A.
Schwarzschild black hole
A Schwarzschild black hole is the simplest theoretical black hole solution in general relativity, describing a static, spherically symmetric, non-rotating, uncharged mass with an event horizon defined by the Schwarzschild radius.
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B.
Bekenstein–Hawking entropy
Bekenstein–Hawking entropy is the thermodynamic entropy associated with a black hole, proportional to the area of its event horizon and fundamental in linking gravity, quantum theory, and thermodynamics.
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C.
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.
-
D.
Einstein field equations
The Einstein field equations are the core mathematical framework of general relativity, relating the curvature of spacetime to the distribution of matter and energy.
-
E.
Higgs boson
The Higgs boson is an elementary particle in the Standard Model whose associated field gives mass to other fundamental particles, confirming a key mechanism of particle physics.
- F. None of above. chosen
Statements (47)
| Predicate | Object |
|---|---|
| instanceOf |
no-hair theorem
ⓘ
theorem in general relativity ⓘ |
| appliesTo | stationary black holes ⓘ |
| assumes |
Einstein field equations
ⓘ
absence of matter fields outside the black hole other than electromagnetic field ⓘ asymptotic flatness of spacetime ⓘ classical, non-quantum description of gravity ⓘ cosmic censorship hypothesis in many formulations ⓘ stationarity ⓘ |
| category |
black hole physics
ⓘ
mathematical relativity ⓘ |
| concerns | classical black holes ⓘ |
| consequence | all stationary, asymptotically flat, electrovac black holes are described by the Kerr–Newman family of solutions ⓘ |
| contrastsWith | dependence on microscopic details of collapsing matter ⓘ |
| excludes | additional classical hair such as higher independent multipole moments ⓘ |
| field | general relativity ⓘ |
| hasExtension | no-hair conjectures for additional fields ⓘ |
| hasImplication | information about infalling matter is not encoded in additional classical observables outside the horizon ⓘ |
| hasLimitation |
does not fully address dynamical or non-stationary black holes
ⓘ
may not apply in non-asymptotically flat spacetimes such as with cosmological constant ⓘ |
| hasNameOrigin | metaphor that black holes have no hair, meaning no additional distinguishing features ⓘ |
| hasStatus | rigorously proven only under specific assumptions ⓘ |
| holdsFor |
charged rotating black holes described by the Kerr–Newman metric
ⓘ
non-rotating uncharged black holes described by the Schwarzschild metric ⓘ uncharged rotating black holes described by the Kerr metric ⓘ |
| implies |
black holes have no additional independent multipole moments beyond those determined by mass, charge, and angular momentum
ⓘ
details of the matter that formed a black hole are not observable from outside except through mass, charge, and angular momentum ⓘ |
| influences |
black hole information paradox
ⓘ
black hole thermodynamics ⓘ |
| involves |
angular momentum dipole moment
ⓘ
electric monopole moment ⓘ mass monopole moment ⓘ |
| isAbout | macroscopic characterization of black holes ⓘ |
| mayBeModifiedBy | quantum effects ⓘ |
| mayFailIn | theories with additional long-range fields ⓘ |
| motivates | search for observational signatures of deviations from Kerr geometry ⓘ |
| parameter |
angular momentum
ⓘ
electric charge ⓘ mass ⓘ |
| relatedConcept |
Israel–Carter–Robinson uniqueness theorems
ⓘ
Kerr–Newman black hole ⓘ |
| relatesTo |
black hole uniqueness theorems
ⓘ
event horizon ⓘ |
| statesThat | a stationary black hole is completely characterized by a small set of macroscopic parameters ⓘ |
| testedBy | ringdown phase observations of binary black hole mergers ⓘ |
| usedIn |
astrophysical modeling of black holes
ⓘ
tests of general relativity with gravitational waves ⓘ |
How these facts were elicited
The pipeline generated the facts above by prompting gpt-5.1 with this entity's name + description and the instruction below.
Instruction
You are a knowledge base construction expert. Given a subject entity and a description of it, return factual statements that you know for the subject as a JSON list of dictionaries(triples), where keys must be "subject", "predicate" and "object". The number of facts may be very high, between 25 to 50 or more, for very popular subjects. For less popular subjects, the number of facts can be very low, like 5 or 10. # Requirements - If you don't know the subject at all, return an empty list. - If the subject is not a named entity, return an empty list. - Include at least one triple where predicate is "instanceOf". - Do not get too wordy. - Separate several objects into multiple triples with one object.
Input
Subject: black hole no-hair theorem Description of subject: The black hole no-hair theorem is a principle in general relativity stating that stationary black holes are completely characterized by only a few macroscopic parameters—mass, electric charge, and angular momentum—regardless of the details of the matter that formed them.
Referenced by (5)
Full triples — surface form annotated when it differs from this entity's canonical label.
this entity surface form:
no-hair theorem
this entity surface form:
no-hair theorem
this entity surface form:
no-hair theorem
this entity surface form:
no-hair theorem for black holes