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.
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 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 black hole
→
Kerr–Newman black hole → 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 |
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
→
|
Referenced by (1)
| Subject (surface form when different) | Predicate |
|---|---|
|
black hole no-hair theorem
→
|
relatedConcept |