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.
Aliases (1)
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
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|
| 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
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|
| mayBeModifiedBy |
quantum effects
→
|
| mayFailIn |
theories with additional long-range fields
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|
| 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 → |
Referenced by (2)
| Subject (surface form when different) | Predicate |
|---|---|
|
Schwarzschild black hole
→
|
obeysLaw |
|
Israel–Carter–Robinson uniqueness theorems
("no-hair theorem")
→
|
relatedTo |