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Physics IV course sequence · Interactive lesson

The Compton shift, derived

Compton's 1923 result is the cleanest evidence that light carries momentum in lumps. Here you build it from scratch: three conservation equations, one unwanted variable to eliminate, and an answer that turns out to depend on the scattering angle and on nothing else — not the wavelength, not the target, not the beam.

UPIV-04.03 · Lesson 3 of 9 in this unit. Position is not a completion score.
Starting model: The Compton shift, derivedA photon of wavelength 71 pm meets an electron at rest at the dot, scatters through 90° and leaves at 73.43 pm; the three arrows are momenta drawn to one scale, and the electron's is the incident momentum minus the scattered one. Below, the same event as a spectrum: the scattered line stands 3.42% of a wavelength to the right of the incident one.arrow length ∝ momentumλ = 71 pm θ = 90°λ′ = 73.43 pmΔλ = 2.426 pmthe electron carries off the restspectrum: displacement from λ, as a fraction of λλ′λ (incident)10%20%
Start with a picture. Change the model in the lab below.
1

Build the model

Two conservation laws, one unwanted angle, and a length worth 2.4263 pm.

The key idea

The Compton shift is the increase in a photon's wavelength when it scatters from a free electron at rest, equal to the Compton wavelength h/mₑ c multiplied by (1 − cos θ), with θ the photon's deflection and no dependence on the incident wavelength.

Example. A 71.10 pm molybdenum Kα X-ray scattered through 90° returns at 71.10 + 2.43 = 73.53 pm, a 3.4% shift; 500 nm green light scattered through the same 90° gains exactly the same amount and comes back at 500.0024 nm.

The complete physical model and assumptions

Treat the X-ray as a particle with energy hc/λ and momentum h/λ, let it strike a free electron sitting at rest, and demand that relativistic energy and both components of momentum balance. That is three equations in four unknowns — the scattered wavelength, the electron's energy, its momentum and its recoil angle — and the invariant E² = (pc)² + (mc²)² supplies the fourth relation. Square and add the two momentum equations, square the energy equation, subtract, and the recoil angle disappears along with the electron's energy, leaving one line: λ′ − λ = (h/mₑ c)(1 − cos θ). A single length survives the algebra, the Compton wavelength h/mₑ c = 2.4263 pm, and it is fixed by the mass of whatever recoils rather than by anything the experimenter chose. The cost of that clean result is the assumption that bought it. A free electron initially at rest is a fiction — real electrons are bound and moving — so the derivation is a limit, trustworthy only when the photon energy dwarfs the binding energy, and it stays silent about how often scattering happens at all. Conservation fixes where the line lands, never how bright it is.

1What the wave picture predicts, and what Compton saw

Classical Thomson scattering has the incident electric field drive the electron into oscillation at the incident frequency, and an oscillating charge radiates at the frequency at which it oscillates. So the scattered light must return at exactly the incident wavelength, at every angle, from every target — the wave account has no free knob with which to change a colour. What Compton measured in 1923, sending 71.10 pm molybdenum Kα X-rays onto graphite, was a second line beside the unshifted one, displaced towards longer wavelengths, with the displacement growing as the detector swung from forward to backward angles and taking the same value whatever the scatterer was made of. No repair to the wave account produces a wavelength change without a moving source. A photon–electron collision does, with nothing left free to adjust.

2Set up the ledger, and name the assumption

Give the photon energy E = hc/λ and momentum p = h/λ, read off the m = 0 branch of the energy–momentum invariant. Put one electron at rest at the origin and let it be free: no lattice, no binding, nothing else available to absorb momentum. Three quantities are then conserved. Energy: hc/λ + mₑ c² = hc/λ′ + Eₑ. Momentum along the beam: h/λ = (h/λ′)cos θ + pₑ cos φ. Momentum across it: 0 = (h/λ′)sin θ − pₑ sin φ. The electron has to be handled relativistically even for modest X-rays, so Eₑ and pₑ are tied together by Eₑ² = (pₑ c)² + (mₑ c²)². Four unknowns, four relations, and the physics stops here — the assumption of a free electron at rest is the entire physical content, and everything that follows is bookkeeping.

3Eliminate the angle nobody measures

The recoil angle φ is in the equations but not in the question. Isolate the electron terms: pₑ cos φ = h/λ − (h/λ′)cos θ and pₑ sin φ = (h/λ′)sin θ. Square both and add. On the left cos²φ + sin²φ = 1 collapses everything to pₑ², and multiplying through by c² gives (pₑ c)² = E² + E′² − 2EE′cos θ. Now take the energy equation in the form Eₑ = E − E′ + mₑ c², square it, and use the invariant to replace Eₑ² − (mₑ c²)² by (pₑ c)²: that route gives (pₑ c)² = (E − E′)² + 2mₑ c²(E − E′). Set the two expressions for (pₑ c)² equal. The E² and E′² terms appear on both sides and cancel, and what survives is 2EE′(1 − cos θ) = 2mₑ c²(E − E′).

4Divide by EE′ and the wavelength form appears

Divide 2EE′(1 − cos θ) = 2mₑ c²(E − E′) through by 2EE′ and the right-hand side becomes a difference of reciprocals: 1 − cos θ = mₑ c²(1/E′ − 1/E). Since E = hc/λ, the reciprocal 1/E is just λ/hc, so mₑ c²(λ′ − λ)/hc = 1 − cos θ, and λ′ − λ = (h/mₑ c)(1 − cos θ). Now read what has vanished. λ is gone from the right-hand side, so 71 pm and 500 nm shift by the same amount. The target material is gone, because only one mass entered and it was the electron's. The intensity never appeared at all. What remains is the angle and a single constant with the dimensions of length, h/mₑ c = 2.4263 pm, multiplied by (1 − cos θ), which runs from 0 forward, through 1 at 90°, to 2 straight back — so no Compton shift can ever exceed 4.8526 pm.

5Absolute, not fractional: why it took X-rays

A spectrometer never measures Δλ on its own; it measures Δλ against the smallest separation λ/R it can resolve at that wavelength, so visibility is set by the ratio Δλ/λ. At 90° that ratio is 2.4263 pm divided by λ. For Compton's 71.10 pm line it is 3.4% — with a crystal spectrometer of resolving power 2000 that is 68 resolution elements, an unmissable displacement. For 500 nm green light the same absolute 2.4263 pm is 4.9 parts per million, so you would need R above 2 × 10⁵ merely to watch the line move, and at a photon energy of 2.5 eV no electron in the target is remotely free anyway. Every optical scattering experiment before 1923 was therefore consistent with no shift at all. The shift is universal; its detectability is not.

6What the free-electron assumption costs

Nothing in the derivation is approximate — granted the assumption, the result is exact. The assumption is the weak point. A real target electron is bound by anything from a few eV to tens of keV and is moving inside the atom. Binding matters once it stops being negligible beside the photon energy: molybdenum Kα at 17.44 keV is sixty-one times carbon's 284 eV K-shell binding, so the free-electron ledger holds and the shifted line is sharp. Push the photon energy down towards the binding energy and the electron can no longer be treated as free; the recoiling body effectively becomes the whole atom, and since the shift goes as 1/m it collapses — that is the origin of the unshifted line, taken up in the next topic. The initial motion of the bound electrons smears the shifted line into a Compton profile. And conservation says nothing at all about how many photons scatter into a given angle: that needs the Klein–Nishina cross-section.

2

Key equations

Read the units, assumptions and limits before substituting.

The Compton shift

Δλ = λ′ − λ = (h/mₑ c)(1 − cos θ)

One line for the whole two-body ledger: hand it θ and it returns the shift, from 0 forward to 2h/mₑ c straight back. Δλ is never negative, so scattering can only redden the photon.

θ is the photon's deflection from the incident direction; λ and λ′ in the same unit of length.

The Compton wavelength of the electron

λC = h/mₑ c = 2.4263 pm

The only length the derivation leaves behind, and it belongs to the recoiling body. Put a proton there instead and it shrinks by 1836, to 1.32 fm.

h = 6.626×10⁻³⁴ J s, mₑ = 9.109×10⁻³¹ kg, c = 2.998×10⁸ m s⁻¹

The conservation ledger

hc/λ + mₑ c² = hc/λ′ + Eₑh/λ = (h/λ′)cos θ + pₑ cos φ0 = (h/λ′)sin θ − pₑ sin φ

The only physics input. Everything after this point is algebra, which is why the result carries no adjustable constant.

Four unknowns λ′, Eₑ, pₑ, φ; the invariant Eₑ² = (pₑ c)² + (mₑ c²)² closes the system.

Eliminating the recoil angle

(pₑ c)² = E² + E′² − 2EE′ cos θ, E = hc/λ, E′ = hc/λ′

The electron's direction never reaches the answer, so the experiment needs to catch only the scattered photon.

Square and add the two momentum equations: cos²φ + sin²φ = 1 removes φ in a single step.

The shift written in energies

E′ = E / [1 + (E/mₑ c²)(1 − cos θ)]

The form a detector that reads energies rather than wavelengths needs: a 511 keV photon deflected through 90° comes back at exactly half its energy, 255.5 keV.

mₑ c² = 511 keV. Identical content to the wavelength form, since E = hc/λ.

Absolute shift, fractional visibility

Δλ/λ = (λC/λ)(1 − cos θ) ≤ 2λC/λ

That ceiling is 6.8% of a 71 pm X-ray but 10 parts per million of 500 nm light, and an instrument weighs Δλ against λ, never against zero.

Ceiling reached at θ = 180°: 4.8526 pm added, whatever λ was.
3

Interactive lab

Predict first. Explore the model. Compare the result.

Explore the model

90 °
0 to 180 °; steps of 5.
71 pm
20 to 220 pm; steps of 1.

Try this. Hold θ at 180°, where the shift hits its ceiling of 4.85 pm, then drag λ from 20 pm to 220 pm: the shift readout never moves, while the line below slides back towards the incident one, from 24% of a wavelength to 2%. That gap is why Compton needed X-rays.

Live results

SHIFT Δλ
2.426 pm
SCATTERED λ′
73.43 pm
Δλ / λ
3.42 %
ENERGY LOST BY PHOTON
3.30 %

Results follow this lesson’s model and assumptions. Displayed values are rounded.

Interactive Physics IV modelA photon of wavelength 71 pm meets an electron at rest at the dot, scatters through 90° and leaves at 73.43 pm; the three arrows are momenta drawn to one scale, and the electron's is the incident momentum minus the scattered one. Below, the same event as a spectrum: the scattered line stands 3.42% of a wavelength to the right of the incident one.arrow length ∝ momentumλ = 71 pm θ = 90°λ′ = 73.43 pmΔλ = 2.426 pmthe electron carries off the restspectrum: displacement from λ, as a fraction of λλ′λ (incident)10%20%
A photon of wavelength 71 pm meets an electron at rest at the dot, scatters through 90° and leaves at 73.43 pm; the three arrows are momenta drawn to one scale, and the electron's is the incident momentum minus the scattered one. Below, the same event as a spectrum: the scattered line stands 3.42% of a wavelength to the right of the incident one.

Predict → change one variable → check

Plan a change before running it. Every other input stays at the saved baseline.

Saved baseline. Scattering angle θ: 90 °; Incident wavelength λ: 71 pm

Baseline 90; choose 0 to 180, in steps of 5.
4. Compared with the saved baseline, this result will…

This experiment is kept only while this page is open. It does not change saved course progress.

4

Catch the common trap

The universal quantity is Δλ, not the fraction of anything. Students who memorise 'the wavelength increases by 2.4 pm' often slide into treating the shift as a percentage — writing that 500 nm green light returns at 517 nm because 2.4263/71.10 is 3.4% — or assume the energy loss must be equally universal. Both readings fail. Δλ is a fixed length added to λ, so the fraction of energy the photon surrenders is Δλ/λ′, and that depends on λ very strongly: at 90° a 71 pm X-ray gives up 3.3% of its energy, while a 1.24 pm photon of 1 MeV gives up 66%, because the same 2.4263 pm swallows most of it. One line, universal; its consequences, anything but.

5

Practice & worked examples

3 authored examples. Make an attempt, then reveal the reasoning one step at a time.

EasyExample 1

A molybdenum Kα beam of wavelength 71.10 pm scatters from the loosely bound electrons in graphite, and a detector sits at θ = 60°. Find the wavelength shift, the scattered wavelength, and the shift as a percentage of the incident wavelength.

Sketch your answer or reasoning, then compare it with the authored solution. Your writing is not automatically graded or saved.

0 of 4 steps revealed.

MediumExample 2

In a repeat of Compton's experiment the incident line is at 71.10 pm and the detector — at an angle the student forgot to record — shows the shifted line at 74.55 pm. Recover the scattering angle, then find the photon energy before and after the collision and the energy handed to the electron.

Sketch your answer or reasoning, then compare it with the authored solution. Your writing is not automatically graded or saved.

0 of 5 steps revealed.

HardExample 3

A spectrometer separates two lines only when they differ by more than λ/R, with resolving power R = 2000. (a) What is the longest incident wavelength whose Compton shift such an instrument could still resolve? (b) Convert that wavelength to a photon energy. (c) Compton nevertheless worked at 71 pm, some 140 times shorter. Say why.

Sketch your answer or reasoning, then compare it with the authored solution. Your writing is not automatically graded or saved.

0 of 5 steps revealed.

6

Quick check

Select an answer and explain it before checking.

The same graphite target is illuminated first with 71.10 pm molybdenum Kα X-rays and then with 500 nm green light, and in each case the scattered light is examined at θ = 90°. What does the Compton formula predict?
7

Review & continue

The Compton shift is the increase in a photon's wavelength when it scatters from a free electron at rest, equal to the Compton wavelength h/mₑ c multiplied by (1 − cos θ), with θ the photon's deflection and no dependence on the incident wavelength.

  • Explain the relationship without looking at the equation.
  • Check a sign, a unit and a model assumption in your working.
  • Return to the lab or worked example if a step is still unclear.

Extra challenging questions

Connect several ideas, explore supplied data, and compare your reasoning with a worked solution.