Israel–Carter–Robinson uniqueness theorems
E43149
The Israel–Carter–Robinson uniqueness theorems are a set of results in general relativity showing that stationary, asymptotically flat black holes in four-dimensional spacetime are completely characterized by just their mass, charge, and angular momentum.
All labels observed (1)
| Label | Occurrences |
|---|---|
| Israel–Carter–Robinson uniqueness theorems canonical | 1 |
How this entity was disambiguated
This entity first appeared as the object of triple T340084 — 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.
Target entity: Israel–Carter–Robinson uniqueness theorems Context triple: [black hole no-hair theorem, relatedConcept, Israel–Carter–Robinson uniqueness theorems]
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A.
Hilbert’s Nullstellensatz
Hilbert’s Nullstellensatz is a foundational theorem in algebraic geometry that establishes a deep correspondence between ideals in polynomial rings and algebraic sets, linking algebra and geometry.
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B.
Nash embedding theorem
The Nash embedding theorem is a fundamental result in differential geometry that shows any Riemannian manifold can be isometrically embedded into some Euclidean space, thereby realizing abstract curved spaces as concrete subsets of standard Euclidean space.
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C.
Dyson’s transform in number theory
Dyson’s transform in number theory is a combinatorial technique introduced by Freeman Dyson to manipulate and relate integer partitions, particularly in the study of partition identities and congruences.
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D.
Janet–Cartan theorem
The Janet–Cartan theorem is a fundamental result in differential geometry stating that any real-analytic Riemannian manifold can be locally isometrically embedded into a Euclidean space of sufficiently high dimension.
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E.
Hilbert problems
The Hilbert problems are a famous list of 23 unsolved mathematical problems presented by David Hilbert in 1900 that profoundly influenced the development of 20th-century mathematics.
- F. None of above. chosen
- G. Unsure - the case is ambiguous/there is not enough information to decide.
Target entity: Israel–Carter–Robinson uniqueness theorems Target entity description: The Israel–Carter–Robinson uniqueness theorems are a set of results in general relativity showing that stationary, asymptotically flat black holes in four-dimensional spacetime are completely characterized by just their mass, charge, and angular momentum.
-
A.
Hilbert’s Nullstellensatz
Hilbert’s Nullstellensatz is a foundational theorem in algebraic geometry that establishes a deep correspondence between ideals in polynomial rings and algebraic sets, linking algebra and geometry.
-
B.
Nash embedding theorem
The Nash embedding theorem is a fundamental result in differential geometry that shows any Riemannian manifold can be isometrically embedded into some Euclidean space, thereby realizing abstract curved spaces as concrete subsets of standard Euclidean space.
-
C.
Dyson’s transform in number theory
Dyson’s transform in number theory is a combinatorial technique introduced by Freeman Dyson to manipulate and relate integer partitions, particularly in the study of partition identities and congruences.
-
D.
Janet–Cartan theorem
The Janet–Cartan theorem is a fundamental result in differential geometry stating that any real-analytic Riemannian manifold can be locally isometrically embedded into a Euclidean space of sufficiently high dimension.
-
E.
Hilbert problems
The Hilbert problems are a famous list of 23 unsolved mathematical problems presented by David Hilbert in 1900 that profoundly influenced the development of 20th-century mathematics.
- F. None of above. chosen
Statements (49)
| Predicate | Object |
|---|---|
| instanceOf |
black hole uniqueness theorem
ⓘ
theorem in general relativity ⓘ |
| appliesTo |
asymptotically flat spacetimes
ⓘ
four-dimensional spacetime ⓘ stationary black holes ⓘ |
| assumes |
Einstein–Maxwell equations
ⓘ
surface form:
Einstein–Maxwell theory
asymptotic flatness ⓘ four spacetime dimensions ⓘ non-degenerate event horizon ⓘ regularity of the event horizon ⓘ stationarity ⓘ vacuum or electrovacuum outside the black hole ⓘ |
| characterizesBy |
angular momentum
ⓘ
electric charge ⓘ mass ⓘ |
| concerns |
Kerr metric
ⓘ
surface form:
Kerr black hole
Kerr–Newman black hole ⓘ Reissner–Nordström metric ⓘ
surface form:
Reissner–Nordström black hole
Schwarzschild black hole ⓘ axisymmetric black holes ⓘ classical black holes ⓘ event horizons ⓘ stationary axisymmetric solutions ⓘ stationary solutions of Einstein–Maxwell equations ⓘ |
| dimension | 4 ⓘ |
| excludes |
black holes with non-Abelian gauge fields
ⓘ
black holes with scalar hair ⓘ higher-dimensional black holes ⓘ non-asymptotically flat black holes ⓘ |
| field | general relativity ⓘ |
| historicalPeriod | late 1960s and early 1970s ⓘ |
| implies |
no-hair property of black holes
ⓘ
uniqueness of the Kerr solution for rotating uncharged black holes ⓘ uniqueness of the Kerr–Newman family for rotating charged black holes ⓘ |
| influenced | modern black hole classification ⓘ |
| involves |
Einstein field equations
ⓘ
global methods in differential geometry ⓘ properties of Killing vector fields ⓘ |
| language | mathematical physics ⓘ |
| namedAfter |
Brandon Carter
ⓘ
David C. Robinson ⓘ Werner Israel ⓘ |
| relatedTo |
black hole no-hair theorem
ⓘ
surface form:
no-hair theorem
|
| requires | axisymmetry for rotating black holes ⓘ |
| statesThat |
a static, asymptotically flat electrovacuum black hole is the Reissner–Nordström solution
ⓘ
a static, asymptotically flat vacuum black hole is the Schwarzschild solution ⓘ a stationary, axisymmetric, asymptotically flat electrovacuum black hole is a Kerr–Newman solution ⓘ |
| typeOf | uniqueness theorem ⓘ |
| validIn | classical general relativity ⓘ |
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Subject: Israel–Carter–Robinson uniqueness theorems Description of subject: The Israel–Carter–Robinson uniqueness theorems are a set of results in general relativity showing that stationary, asymptotically flat black holes in four-dimensional spacetime are completely characterized by just their mass, charge, and angular momentum.
Referenced by (1)
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