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.

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All labels observed (4)

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

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 ⓘ