
Optional unit · institution-dependent · Interactive lesson
Relativistic Doppler shift and aberration
Light from a moving source is shifted twice over: its clock runs slow, and successive wavefronts leave from different places. Learn to combine those two effects at any angle, read a star's radial velocity from its lines, and predict the redshift that appears even when the source is neither approaching nor receding.
UPIII-08.06 · Lesson 6 of 9 in this unit. Position is not a completion score.Optional unit · institution-dependent. This modern-physics material is an introductory survey, not a complete course in relativity, quantum, atomic, nuclear or particle physics. Your university determines the required depth and assessment. Optional work is not a required completion gate.
Build the model
A moving clock ticks slowly, and every tick has a different distance to travel.
The key idea
The relativistic Doppler shift is the ratio of received to emitted frequency, f/f₀ = 1/[γ(1 − β cos θ)], fixed by the source's speed β = v/c and the observer-frame angle θ between its velocity and the light's path to the observer.
Example. A source receding head-on at 0.60c has γ = 1.25 and 1 + β = 1.60, so f/f₀ = 1/(1.25 × 1.60) = 0.50 and a 500 nm line arrives at 1000 nm; seen at closest approach, the same source gives f/f₀ = 1/γ = 0.80, so the line arrives at 625 nm.
The complete physical model and assumptions
Classical Doppler needs two formulas — f₀/(1 − β) for a moving source and f₀(1 + β) for a moving observer — because sound has a medium that decides who is really moving. Light in vacuum has none, and the first postulate forbids the asymmetry: only the relative velocity can matter. A dilated source clock supplies it. Wavefronts emitted every T₀ in the source's own frame are emitted every γT₀ in the observer's, and the source shifts by vγT₀ between them, so the arrival interval is γT₀(1 − β cos θ), where θ is the observer-frame angle between the source's velocity and the light's path to the observer. Head-on this gives f = f₀√((1 + β)/(1 − β)), the geometric mean of the two classical answers: it agrees with both to first order in β and differs at β²/2, the term Ives and Stilwell measured in 1938. At θ = 90° the light-travel factor 1 − β cos θ is exactly 1 and only time dilation remains, f = f₀/γ, a redshift with no classical counterpart. The same velocity transformation also tilts the light's direction, cos θ = (cos θ′ + β)/(1 + β cos θ′), which displaces every star by up to 20.5″ over Earth's orbit and throws a fast jet's emission into a forward cone of half-angle about 1/γ. The derivation assumes vacuum propagation with inertial source and observer, and it says nothing about cosmological redshift, which is the stretching of wavelengths by expanding space rather than motion through it.
1Two effects on one moving clock
Let the source emit a wavefront every T₀ = 1/f₀ by its own clock while it recedes from the observer at speed v, and do the bookkeeping in the observer's frame. First, time dilation: the source's clock runs slow, so wavefronts are emitted every γT₀ of observer time. Second, light-travel time: between two emissions the source moves vγT₀ farther away, so the second wavefront has that much more path and arrives a further vγT₀/c behind. The arrival interval is T = γT₀(1 + β), so f = f₀/[γ(1 + β)]. Now tidy the algebra: 1/γ = √(1 − β²) = √((1 − β)(1 + β)), and dividing by (1 + β) leaves f = f₀√((1 − β)/(1 + β)). For approach the path shrinks instead, the sign in the bracket flips, and f = f₀√((1 + β)/(1 − β)). At β = 0.60, γ = 1.25 and the factors are 1/(1.25 × 1.60) = 0.50 for recession and 1/(1.25 × 0.40) = 2.00 for approach. Wavelength scales the other way, λ = c/f, so a receding source at 0.60c stretches every wavelength by exactly 2.
2Why relativity needs only one formula
For sound, a source approaching a fixed listener gives f₀/(1 − β), while a listener approaching a fixed source gives f₀(1 + β), with β the speed over the speed of sound: different numbers, because the air decides who is moving. Light in vacuum has no medium, and the principle of relativity forbids any experiment that tells 'source moving' from 'observer moving'. The relativistic factor √((1 + β)/(1 − β)) is the geometric mean of the two classical answers, √[(1 + β) × 1/(1 − β)], and it is the one answer both frames can share. Expand it: 1 + β + β²/2 + β³/2 + …. The classical forms are 1 + β and 1 + β + β² + …, so all three agree at first order and the relativistic one splits the difference at second order. At β = 0.10 they predict 1.1000, 1.1111 and 1.1055. Ives and Stilwell (1938) isolated that β²/2 term with hydrogen ions at β ≈ 0.005, viewing the beam head-on and in a mirror at once: the mean of the blue- and red-shifted lines sits at γλ₀, so the first-order shifts cancel and only the time-dilation remainder survives.
3At any angle, the light-travel term carries a cosine
Let the source move along a direction making angle θ, in the observer's frame, with the light's path to the observer: θ = 0 is head-on approach and 180° is direct recession. Between two emissions γT₀ apart the source moves vγT₀, and the component of that displacement along the line of sight, vγT₀ cos θ, is the amount by which the second wavefront's path is shorter — the observer is far enough away that the two paths are parallel. The arrival interval is therefore γT₀(1 − β cos θ), and f = f₀/[γ(1 − β cos θ)]. Two factors do two jobs: the 1/γ is time dilation and never changes sign; the bracket is the light-travel term, blue for cos θ > 0 and red for cos θ < 0. They cancel where 1 − β cos θ₀ = 1/γ, that is cos θ₀ = (1 − 1/γ)/β. At β = 0.80, γ = 5/3 and cos θ₀ = 0.40/0.80 = 0.50, so θ₀ = 60°: a source still moving partly towards you shows no shift, and every angle beyond 60° is redshifted. Dimensions check — β and cos θ are pure numbers, so f carries the unit of f₀ — and the limit β → 0 returns f = f₀ at every angle.
4Transverse Doppler: a shift with no classical analogue
Set θ = 90° in the observer's frame. The light was emitted from the point of closest approach, the light-travel term is exactly 1, and f = f₀/γ. Nothing about the path is changing; the shift is pure time dilation, and classical physics predicts none. Be careful which frame owns the right angle. Written with the emission angle θ′ in the source's frame the same physics reads f = f₀γ(1 + β cos θ′), and at θ′ = 90° the observer sees a blueshift of γ, because that light arrives from ahead of the source, at cos θ = β. Both statements are correct; they describe different photons. The cleanest measurement uses a source emitting in two opposite directions at once, such as the twin jets of the microquasar SS 433 at β ≈ 0.26. The approaching and receding jets show wavelengths λ₀γ(1 − β cos θ) and λ₀γ(1 + β cos θ), whose mean is γλ₀ whatever θ is, so the midpoint of the two lines sits redward of the rest wavelength by z̄ = γ − 1 ≈ 0.036 — the transverse effect read straight off a spectrum.
5Aberration: the same transformation tilts the light
In the source's frame a photon leaves at angle θ′ to the x-axis with velocity components (c cos θ′, c sin θ′). The source frame moves at +v along x relative to the observer, so the velocity transformation of the previous topic gives uₓ = (c cos θ′ + v)/(1 + β cos θ′), and because the speed is still c, cos θ = (cos θ′ + β)/(1 + β cos θ′). A photon emitted sideways in the source frame, θ′ = 90°, is seen at cos θ = β: thrown forward. Half of an isotropic source's photons therefore arrive inside a cone of half-angle θ½ with sin θ½ = √(1 − β²) = 1/γ — 36.9° at β = 0.80, and 5.7° for a jet knot with γ = 10. This beaming, compounded by the blueshift of each photon and the bunching of their arrival times, is why an approaching jet outshines its receding twin; nothing about what the jet emits has changed. The effect exists at any speed. Earth's orbital speed of 29.8 km s⁻¹ gives β = 9.94 × 10⁻⁵, an angular displacement of β rad = 20.5″, and every star traces an ellipse of that semi-major axis through the year — Bradley's aberration of 1729, the first direct evidence that Earth moves. As β → 0 the formula returns θ = θ′, as it must.
6Reading a spectrum, and where the formula stops
A star's radial velocity comes from a line whose rest wavelength λ₀ is known. Write z = λ/λ₀ − 1; for β ≪ 1, z ≈ β and vᵣ ≈ cz, with a fractional error of β/2, of order 10⁻⁴ or less at typical stellar speeds of tens of km s⁻¹. A Hα line at 656.28 nm observed at 656.42 nm gives z = 2.13 × 10⁻⁴ and vᵣ = 64 km s⁻¹, receding — the number whose periodic wobble reveals binary companions and planets. When β is not small the inverse formula β = ((1 + z)² − 1)/((1 + z)² + 1) is compulsory: z = 0.5 means β = 0.385, not 0.5, and z = 2 means β = 0.80, not a speed above c. Then the boundaries. The derivation assumed vacuum, where the wave speed is c in both frames; in a medium the phase speed differs and the formula changes. It assumed inertial source and observer, so only the instantaneous velocity at emission enters for anything accelerating. And it does not describe cosmological redshift: a galaxy at z = 2 is not moving through space at 0.80c; its light has been stretched by expanding space, and turning that z into a distance belongs to cosmology, not to this formula.
Key equations
Read the units, assumptions and limits before substituting.
Longitudinal Doppler, head-on approach
f = f₀ √((1 + β)/(1 − β))
Symmetric between source and observer: only the relative speed enters, unlike the two classical formulas for sound.
f₀ the frequency in the source's rest frame (Hz), β = v/c dimensionless; invert the root for recessionDoppler shift at any angle
f = f₀ / [γ (1 − β cos θ)]
θ = 0 and 180° recover the longitudinal factors; the 1/γ is time dilation and the bracket is the light-travel term.
θ: observer-frame angle between the source velocity and the light's path to the observer; γ = 1/√(1 − β²)Transverse Doppler shift
f = f₀ / γ (θ = 90° in the observer's frame)
A redshift with no classical analogue: the path length is momentarily constant, and only the clock rate remains.
Light received from the point of closest approach; in the source's frame that light left at cos θ′ = −βRadial speed from a measured redshift
β = ((1 + z)² − 1)/((1 + z)² + 1)
For β ≪ 1 this is v ≈ cz, high by a fraction β/2; at z = 0.5 the exact form gives β = 0.385, not 0.5.
z = λ/λ₀ − 1 = √((1 + β)/(1 − β)) − 1 for head-on recession; z and β are dimensionlessAberration of light
cos θ = (cos θ′ + β)/(1 + β cos θ′)
Light emitted sideways in the source frame (θ′ = 90°) arrives from cos θ = β: a fast source beams its light forward.
θ′ the emission angle in the source frame, θ the angle in the observer frame, both measured from the source's velocityLow-speed expansion
√((1 + β)/(1 − β)) = 1 + β + β²/2 + β³/2 + …
First order is the classical shift; β²/2 is the time-dilation correction Ives and Stilwell measured in 1938.
Dimensionless; compare the classical 1 + β (moving observer) and 1 + β + β² + … (moving source)Interactive lab
Predict first. Explore the model. Compare the result.
Explore the model
Try this. Set θ to 90° and drag β upward: the open dot stays pinned at f = f₀ while the solid dot sinks to 1/γ = {√(1-β*β)|3}, the transverse redshift. Then find where the solid curve crosses the f = f₀ line: θ₀ = {deg(acos(clamp((1-√(1-β*β))/max(β,0.01),-1,1)))|1}°, always short of 90°.
Live results
- f/f₀ AT θ
- 0.800
- TRANSVERSE 1/γ
- 0.800
- ZERO-SHIFT ANGLE θ₀
- 70.5 °
- SOURCE-FRAME ANGLE θ′
- 126.9 °
Results follow this lesson’s model and assumptions. Displayed values are rounded.
Predict → change one variable → check
Plan a change before running it. Every other input stays at the saved baseline.
Saved baseline. Source speed β = v/c: 0.60; Observer-frame angle θ: 90 °
This experiment is kept only while this page is open. It does not change saved course progress.
Catch the common trap
First-year Doppler is about path length, so students conclude that light received from the point of closest approach — where the distance is momentarily constant — carries no shift, and that a 'transverse' source shows f = f₀. It shows f₀/γ. The wavefront interval is set by two things, the changing path and the rate of the emitting clock, and at closest approach only the first switches off. Time dilation never does: the source's clock runs slow in the observer's frame whatever direction it moves, so the whole f/f₀ curve is displaced towards the red by 1/γ and the zero-shift angle sits short of 90°, at cos θ₀ = (1 − 1/γ)/β. The companion mistake is to treat 'transverse' as frame-independent: light emitted at 90° in the source's own frame arrives from cos θ = β in the observer's frame and is blueshifted by γ.
Practice & worked examples
3 authored examples. Make an attempt, then reveal the reasoning one step at a time.
EasyExample 1
The Hα line of hydrogen has rest wavelength 656.28 nm. In the spectrum of a nearby star it is measured at 656.42 nm. Find the star's radial velocity, state its direction, and decide whether the relativistic form of the Doppler formula changes the answer.
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.
- The line is shifted to longer wavelength, so the star is receding. Redshift: z = (656.42 − 656.28)/656.28 = 0.14/656.28 = 2.133 × 10⁻⁴.
- For small β the factor √((1 + β)/(1 − β)) = 1 + β + β²/2 + … reduces to 1 + z ≈ 1 + β, so β ≈ z and vᵣ ≈ cz = 2.998 × 10⁸ m s⁻¹ × 2.133 × 10⁻⁴ = 6.40 × 10⁴ m s⁻¹.
- Exact inversion: β = ((1 + z)² − 1)/((1 + z)² + 1) = 4.2669 × 10⁻⁴/2.00043 = 2.1330 × 10⁻⁴, the same to four figures. The β²/2 term lowers vᵣ by a fraction β/2 ≈ 1 × 10⁻⁴, about 7 m s⁻¹.
- The shift itself is known only to ±0.01 nm out of 0.14 nm, about 7%, or ±5 km s⁻¹. The relativistic correction is several hundred times smaller than the measurement uncertainty.
Answer. vᵣ ≈ 64 km s⁻¹, receding. The relativistic correction is about 7 m s⁻¹, far below the ±5 km s⁻¹ set by the 0.01 nm wavelength resolution.
MediumExample 2
A source emitting at f₀ = 5.00 × 10¹⁴ Hz (600 nm) moves at 0.60c past an observer. Find the received frequency (a) for head-on approach, (b) for direct recession, (c) for light emitted at closest approach in the observer's frame, and (d) the observer-frame angle at which no shift is seen.
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.
- β = 0.60, so γ = 1/√(1 − 0.36) = 1/0.80 = 1.25. All four parts use f = f₀/[γ(1 − β cos θ)] with θ measured in the observer's frame from the source velocity to the light's path.
- (a) θ = 0: f = 5.00 × 10¹⁴/(1.25 × 0.40) = 1.00 × 10¹⁵ Hz, a factor 2.00 — equally √(1.60/0.40) = √4. The 600 nm line arrives at 300 nm, in the ultraviolet.
- (b) θ = 180°: f = 5.00 × 10¹⁴/(1.25 × 1.60) = 2.50 × 10¹⁴ Hz, the reciprocal factor 0.50: 600 nm arrives at 1200 nm, in the infrared.
- (c) θ = 90°: f = f₀/γ = 5.00 × 10¹⁴/1.25 = 4.00 × 10¹⁴ Hz, a redshift to 750 nm although the distance is momentarily constant.
- (d) f = f₀ requires 1 − β cos θ₀ = 1/γ, so cos θ₀ = (1 − 0.80)/0.60 = 0.333 and θ₀ = 70.5°. Check either side: θ = 60° gives 1/(1.25 × 0.70) = 1.14, still blue; θ = 80° gives 1/(1.25 × 0.896) = 0.893, red.
Answer. (a) 1.00 × 10¹⁵ Hz, (b) 2.50 × 10¹⁴ Hz, (c) 4.00 × 10¹⁴ Hz, (d) θ₀ = 70.5°; every observer-frame angle beyond 70.5° is redshifted.
HardExample 3
A microquasar ejects two identical jets in opposite directions at the same speed. Their Hα emission (rest wavelength 656.28 nm) is observed at 584.8 nm from one jet and 791.2 nm from the other. Taking the jets as inertial, find the jet speed β, the angle θ between the approaching jet and the line of sight, and the angle in the approaching jet's own frame at which the received light was emitted.
Sketch your answer or reasoning, then compare it with the authored solution. Your writing is not automatically graded or saved.
0 of 6 steps revealed.
- Let θ be the observer-frame angle between the approaching jet's velocity and the line of sight. From f = f₀/[γ(1 − β cos θ)], λₐ = λ₀γ(1 − β cos θ); the receding jet moves at 180° − θ, so λᵣ = λ₀γ(1 + β cos θ).
- Adding removes the cosine: (λₐ + λᵣ)/2 = γλ₀, so γ = (584.8 + 791.2)/(2 × 656.28) = 688.0/656.28 = 1.0483. The midpoint of the two lines is redshifted by z̄ = γ − 1 = 0.048 whatever the orientation — the transverse Doppler shift measured directly.
- β = √(1 − 1/γ²) = √(1 − 0.9099) = √0.0901 = 0.300, so the jets move at 0.30c = 9.0 × 10⁷ m s⁻¹.
- Subtracting isolates the cosine: (λᵣ − λₐ)/(2λ₀) = γβ cos θ = 206.4/1312.56 = 0.1572, so β cos θ = 0.1572/1.0483 = 0.1500 and cos θ = 0.500: θ = 60.0°.
- Aberration for the light received from the approaching jet: cos θ′ = (cos θ − β)/(1 − β cos θ) = (0.500 − 0.300)/(1 − 0.150) = 0.235, so θ′ = 76.4°. In the jet's frame that light left 16° further back than the observer sees it: the jet beams its emission forward.
- Checks: the approaching jet's frequency is boosted by 1/[γ(1 − 0.150)] = 1.122 and the receding one's reduced by 1/[γ(1.150)] = 0.829; their ratio 1.353 equals 1.150/0.850, and both formulas return f₀ as β → 0.
Answer. β = 0.300 (v = 9.0 × 10⁷ m s⁻¹), θ = 60.0° to the line of sight, and the received light left the approaching jet at θ′ = 76.4° in its own frame.
Quick check
Select an answer and explain it before checking.
Review & continue
The relativistic Doppler shift is the ratio of received to emitted frequency, f/f₀ = 1/[γ(1 − β cos θ)], fixed by the source's speed β = v/c and the observer-frame angle θ between its velocity and the light's path to the observer.
- 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.