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Momentum Density in Electromagnetic Fields

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Electromagnetic Field Energy and ConservationPoynting Vector and Electromagnetic Energy Flow+1 moreAngular Momentum Density in Electromagnetic FieldsMaxwell Stress Tensor and Field Forces
momentum-density radiation-pressure field-momentum

Core Idea

Electromagnetic fields carry momentum density g = S/c² = (ε₀/c²)(E × B), where S is the Poynting vector. This momentum transfers to matter in the form of radiation pressure, with magnitude equal to energy density divided by c².

Explainer

You've already established from the Poynting vector that electromagnetic fields carry energy, with energy flux S = (1/μ₀)(E × B) measured in watts per square meter. The deeper and perhaps more surprising result is that fields also carry momentum. This isn't obvious classically — momentum seems like a property of matter — but it follows inescapably from the requirement that momentum be conserved when light interacts with matter.

Here's the argument: when an electromagnetic wave hits an absorbing surface and the charges in the surface begin to move, the Lorentz force F = q(E + v×B) has two parts. The electric field accelerates the charges, and then the magnetic field exerts a force on those moving charges. This secondary magnetic force is directed along the propagation direction of the wave — it pushes the surface forward. Something must be carrying that momentum before the wave is absorbed, and that something is the field itself. The momentum density is g = S/c² = ε₀(E × B), pointing in the same direction as the energy flow, with magnitude equal to the energy density divided by c.

The transfer of field momentum to matter is called radiation pressure. For a plane wave with energy density u, the radiation pressure on a perfect absorber is P = u (in SI units of N/m²), and on a perfect reflector it's P = 2u (because the momentum reverses). These are tiny forces in everyday life — the radiation pressure of sunlight on Earth is about 5 μPa — but they become significant in astrophysics (stellar winds blow material away from stars), in optical trapping (laser tweezers grip microscopic beads), and in proposed solar sail spacecraft.

The relationship g = S/c² has a profound implication: energy and momentum in electromagnetic fields are not independent, but tied by g = u/c = energy/(c·volume). This is exactly the relationship for massless particles, and it foreshadows the photon picture in quantum mechanics — photons carry energy E = hf and momentum p = h/λ = E/c. The classical result for field momentum per unit volume matches the quantum mechanical count of photon momenta, confirming that even the classical field theory anticipates the quantum nature of light.

Practice Questions 5 questions

Prerequisite Chain

Understanding ZeroThe Number ZeroCounting to FiveCounting to 10Counting to 20Counting a Set of Objects Up to 20Cardinality: The Last Number CountedMatching Numerals to QuantitiesSubitizing Small QuantitiesAddition Within 10Number Bonds to 10Addition Within 20Doubles and Near DoublesDoubles Facts Within 10Near Doubles Facts Within 20Mental Math Strategies for AdditionMental Math: Adding and Subtracting TensAddition Within 100Repeated Addition as MultiplicationMultiplication as Equal GroupsMultiplication: ArraysBasic Multiplication Facts (0s, 1s, 2s, 5s, 10s)Multiplication Facts Within 100Division as Equal SharingDivision as Grouping (Measurement Division)Division: Grouping (Repeated Subtraction) ModelDivision: Fair Sharing ModelDivision as Equal SharingDivision as GroupingBasic Division FactsDivision Facts Within 100Multiplication and Division Fact FamiliesRelationship Between Multiplication and DivisionDivision Facts as Inverse of MultiplicationRemainders and Quotients in DivisionDivision Word ProblemsMulti-Step Word ProblemsSolving Multi-Step Word ProblemsMultiplication Word ProblemsDivision Word ProblemsIntroduction to Long DivisionFactors and MultiplesPrime and Composite NumbersEquivalent FractionsRelating Fractions and DecimalsDecimal Place ValueIntegers and the Number LineComparing and Ordering IntegersAbsolute ValueAdding IntegersSubtracting IntegersMultiplying IntegersDividing IntegersUnit RatesProportionsPercent ConceptConverting Between Fractions, Decimals, and PercentsOperations with Rational NumbersTwo-Step EquationsSolving Multi-Step EquationsEquations with Variables on Both SidesAngle Pairs: Complementary, Supplementary, and VerticalParallel Lines and TransversalsCorresponding AnglesAlternate Interior AnglesTriangle Angle Sum TheoremExterior Angle TheoremTriangle Inequality TheoremSimilar Triangles: AA SimilaritySimilar Triangles: SSS and SAS SimilarityProportions in Similar TrianglesRight Triangle Trigonometry IntroductionSine, Cosine, and Tangent RatiosTrigonometric Ratios ReviewRadian MeasureConverting Between Degrees and RadiansThe Unit CircleGraphing Sine and CosineGraphing Tangent and Reciprocal Trigonometric FunctionsDerivatives of Trigonometric FunctionsAntiderivativesIndefinite IntegralsBasic Integration RulesRiemann SumsDefinite Integral DefinitionDouble Integrals: Definition and SetupIterated Integrals and Fubini's TheoremDouble Integrals over Rectangular RegionsDouble Integrals over General RegionsApplications of Double Integrals: Area, Mass, and MomentsCenter of MassConservation of Linear MomentumElastic CollisionsInelastic CollisionsCoefficient of RestitutionCollision Analysis and Real-World ApplicationsTwo-Body Collisions in the Center-of-Mass FrameReduced Mass and Two-Body ProblemsKinematics in Two DimensionsProjectile MotionCircular Motion: KinematicsCircular Motion: Dynamics and Centripetal ForceMagnetic Dipole Moment from Current LoopsForce on Current-Carrying Conductors in Magnetic FieldsBiot-Savart LawAmpère's LawMagnetic Flux and Electromagnetic InductionFaraday's Law of Electromagnetic InductionFaraday's Law of InductionMaxwell's Equations in Integral FormMaxwell's Equations in Differential FormDerivation of the Electromagnetic Wave EquationPlane Electromagnetic WavesPoynting Vector and Electromagnetic Energy FlowElectromagnetic Angular MomentumMomentum Density in Electromagnetic Fields

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