Kerr–Newman black hole

E43148

asymptotically flat spacetime black hole solution exact solution of Einstein field equations rotating charged black hole stationary axisymmetric spacetime type D Petrov spacetime

The Kerr–Newman black hole is a theoretical solution of Einstein’s field equations describing a rotating, electrically charged black hole characterized solely by its mass, angular momentum, and charge.

Try in SPARQL Jump to: Surface forms Disambiguation Statements Elicitation Referenced by

All labels observed (4)

Label	Occurrences
Kerr–Newman metric	5
Kerr–Newman black hole canonical	3
Kerr–Newman spacetime	2
Kerr–Newman solution	1

How this entity was disambiguated

This entity first appeared as the object of triple T340062 — 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: Kerr–Newman black hole
Context triple: [black hole no-hair theorem, relatedConcept, Kerr–Newman black hole]

A. 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.
B. Kerr metric
The Kerr metric is the exact general relativity solution describing the spacetime geometry around a rotating, uncharged black hole.
C. 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.
D. Reissner–Nordström metric
The Reissner–Nordström metric is an exact solution in general relativity describing the spacetime geometry outside a static, spherically symmetric, electrically charged black hole.
E. Kruskal–Szekeres coordinates
Kruskal–Szekeres coordinates are a maximal extension coordinate system used in general relativity to smoothly describe the entire spacetime of a Schwarzschild black hole, including regions across the event horizon.
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: Kerr–Newman black hole
Target entity description: The Kerr–Newman black hole is a theoretical solution of Einstein’s field equations describing a rotating, electrically charged black hole characterized solely by its mass, angular momentum, and charge.

A. 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.
B. Kerr metric
The Kerr metric is the exact general relativity solution describing the spacetime geometry around a rotating, uncharged black hole.
C. 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.
D. Reissner–Nordström metric
The Reissner–Nordström metric is an exact solution in general relativity describing the spacetime geometry outside a static, spherically symmetric, electrically charged black hole.
E. Kruskal–Szekeres coordinates
Kruskal–Szekeres coordinates are a maximal extension coordinate system used in general relativity to smoothly describe the entire spacetime of a Schwarzschild black hole, including regions across the event horizon.
F. None of above. chosen

Statements (50)

Predicate	Object
instanceOf	asymptotically flat spacetime ⓘ black hole solution ⓘ exact solution of Einstein field equations ⓘ rotating charged black hole ⓘ stationary axisymmetric spacetime ⓘ type D Petrov spacetime ⓘ
belongsTo	class of electrovacuum solutions ⓘ
canHave	magnetic charge in generalized solutions ⓘ
characterizedBy	electric charge ⓘ mass ⓘ spin ⓘ
definedIn	four-dimensional spacetime ⓘ
describedByTheory	general relativity ⓘ
generalizes	Kerr metric ⓘ surface form: Kerr black hole Reissner–Nordström metric ⓘ surface form: Reissner–Nordström black hole
hasChargeType	electric charge ⓘ
hasConservedQuantity	angular momentum ⓘ electric charge ⓘ mass-energy ⓘ
hasCoordinateSystem	Boyer–Lindquist coordinates ⓘ
hasEffect	Kerr metric ⓘ surface form: Lense–Thirring precession frame dragging ⓘ
hasEventHorizon	inner Cauchy horizon ⓘ outer event horizon ⓘ
hasExtremalCondition	M^2 = a^2 + Q^2 in geometric units ⓘ
hasInnerHorizonRadiusFormula	r_- = M - sqrt(M^2 - a^2 - Q^2) ⓘ
hasLimitingCase	naked singularity when M^2 < a^2 + Q^2 ⓘ
hasOuterHorizonRadiusFormula	r_+ = M + sqrt(M^2 - a^2 - Q^2) ⓘ
hasParameter	angular momentum ⓘ electric charge ⓘ mass ⓘ
hasRegion	ergosphere ⓘ
hasSingularity	ring singularity ⓘ
hasSurface	Killing horizon ⓘ
hasSymmetry	axisymmetry ⓘ stationary symmetry ⓘ
hasThermodynamicProperty	Bekenstein–Hawking entropy ⓘ Hawking radiation ⓘ surface form: Hawking temperature
hasTopology	R^2 × S^2 outside the ring singularity ⓘ
metricType	Kerr–Newman black hole self-linksurface differs ⓘ surface form: Kerr–Newman metric
namedAfter	Ezra Newman ⓘ Roy Kerr ⓘ
obeys	cosmic censorship conjecture when non-extremal ⓘ
reducesTo	Kerr black hole when charge is zero ⓘ Reissner–Nordström black hole when angular momentum is zero ⓘ Schwarzschild black hole ⓘ surface form: Schwarzschild black hole when charge and angular momentum are zero
satisfies	no-hair theorem parameters mass, charge, angular momentum ⓘ
solutionOf	Einstein–Maxwell equations ⓘ
usedIn	studies of black hole thermodynamics ⓘ tests of the no-hair theorem ⓘ

How these facts were elicited