Doppler effect

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## Contents

* 1 Analysis
* 2 Absolute motion
* 3 Other examples
* 4 Notes

The Doppler effect (or Doppler shift, or Doppler's principle), named after Christian Doppler who proposed it in 1842,[1] is the change in frequency of a wave for an observer moving relative to the source of the wave. If the observer and source of wave motion approach each other, the frequency appears higher, and if the observer and the source separate, the frequency appears lower.

## Analysis[edit]

(PD) Image: John R. Brews
Boat traveling against waves experiences Doppler effect.

The increase in frequency when moving toward a source can be explained using the figure. Suppose that waves blowing ashore with velocity c are spaced a distance λ apart. In that case, the time between crests for an observer at a fixed location is λ / c, and the frequency with which a crest appears at a fixed location is fw :

fw=1λ/c=cλ .

The boat going to sea is running at velocity v in the opposite direction to the waves, and toward the source of the wind. Consequently the boat moves relative to the crests at a speed v+c. That means a crest is met at intervals of time τ :

τ=λ(v+c) .

In other words, the frequency with which the boat bumps over a crest fb is:

fb=1τ=1λ/(v+c)=fwv+cc=fw(1+vc) .

so evidently fb is a higher frequency than the frequency fw of the waves themselves. This increase in frequency is the Doppler effect, and it is often expressed as the shift in frequency fd, the Doppler shift, namely:

fd=fb−fw=fwvc .

Of course, if the boat runs inshore with the wave, away from the source of the wind, the opposite happens: it takes the boat longer between crests, and the frequency with which the boat bumps over a crest is lower than the actual frequency of the waves. In particular, if the boat moves at the same speed as the waves (rides the waves into shore) the frequency of bumping over crests drops to zero.

(PD) Image: John R. Brews
Pulse separation for a stationary source (top) and a moving source (bottom)

One might think it immaterial whether the source approached the observer, or the other way around. However, it is not that simple.

The figure at the right shows a source emitting pulses every τ seconds that propagate at a speed c. The distance between pulses when the source is stationary is λs = cτ. However, when the source moves with a speed v, it translates a distance vτ between pulses, moving each pulse closer to its predecessor by this distance, and resulting in a spacing between pulses of λm = (c−v)τ. Consequently the wave with a moving source has a frequency fm related to the frequency when the source is stationary fs as:

fm=fscc−v=fs11−v/c ,

and a Doppler shift fd of

fd=fsv/c1−v/c .

If the source moves as fast as the pulses, so v=c, this frequency becomes infinite, and the interpretation is that the source cannot emit a pulse in the forward direction because it always is moving ahead of the pulse.

In the general case, the observed frequency fo is related to the emission frequency of the source fe as:

fo=fe(1+vo/c1−vs/c) ,

with c the speed of advance of the wave, vo the speed of the observer moving against the wave direction, and vs the speed of the source moving in the wave direction.[2] For positive v’s, that is, with both the observer and the source moving toward each other, both the numerator (>1) and the denominator (<1) increase the observed frequency.

When vo and vs are both much smaller than c, as is typically the case, a useful approximation is

|Δf|f≈|Δv|c,

where Δf is the difference in observed and emitted frequencies, f can be taken to be either the observed or emitted frequency (since they are approximately equal), and Δv is the difference in the velocities of the source and observer (equal to zero when both move in the same direction at the same speed).

Solving the above approximation for |Δf| gives

|Δf|≈|Δv|fc=|Δv|λ

## Absolute motion[edit]

It would appear that careful observation of the Doppler effect could distinguish between movement of the source and that of the observer. But if they are in uniform straight-line motion toward one another, should it be possible to distinguish which object was moving? The answer is "yes, we can tell the difference" in the case where a medium is involved like air or water, because the medium introduces a third reference frame, and the discussion above is made in the frame of the medium. However, in the case of light in a classical vacuum, according to special relativity one cannot detect the medium, so the Doppler shift cannot be given by the above formula.[3] The idea resolving this paradox was pointed out by Einstein; time dilation: when the source or the observer moves, their internal clocks slow down, an effect noticeable as speeds approach the speed of light. In the case of light, the Doppler effect cannot distinguish whether the source or the observer is moving, only that they are approaching each other or separating from each other. Consequently light in classical vacuum is a special case.[4]

An interesting corollary of special relativity is that there is a transverse Doppler effect for light emitted in vacuum, that is, a Doppler effect is present even for an observation perpendicular to the motions of source or observer, sometimes called the second-order Doppler effect because it is of second order, varying as (v/c)2 (c the speed of light in classical vacuum).[5]

## Other examples[edit]

The same effect appears when the ear and a police siren move toward each other: the sound of the siren to the ear is pitched higher than the actual frequency of the siren, and when the police pass, so the ear and siren are separating, and the waves from the siren are traveling in the same direction as the ear, the pitch to the ear drops to become lower than the frequency of the siren.[6]

As for binary stars, the case considered by Doppler, as the stars orbit each other, they are alternately moving toward and away from the observing astronomer, so the frequency of the light from each star (its color) alternates as well.[7] A Doppler effect is seen for stars even when they are in a plane perpendicular to the line of sight, because of the transverse Doppler effect predicted by special relativity.[5] In this example, the light always propagates in the same direction, and only the separation of the observer and source is changing.

## Notes[edit]

1. ↑ C Doppler (1843). "Über das farbige Licht der Doppelsterne und einiger anderer Gestirne des Himmels (On the colored light of the binary stars and some other stars of the heavens)". Abhandlungen der koniglich bohmischen Gesellschaft der Wissenschaften vol 2,: pp. 465-482.
2. ↑ See, for example, Raymond A. Serway, John W. Jewett (2006). “§13.8: The Doppler effect”, Principles of physics: a calculus-based text, Volume 1, 4rth ed. Cengage Learning, pp. 417-419. ISBN 053449143X.
3. ↑ The quantum vacuum is viewed as a medium with various electrodynamic properties such as vacuum polarization, and is spoken of as the modern version of the æther. Motion relative to the quantum vacuum, however, also is beyond detection, as the quantum vacuum is Lorentz invariant. See, for example, Vesselin Petkov (2010). Minkowski Spacetime: A Hundred Years Later. Springer, p. 214. ISBN 9048134749. “…the vacuum is the only Poincaré invariant pure state” A technical description by Dirac is that the quantum vacuum has a velocity subject to uncertainty relations, and a perfect vacuum state equalizes the velocity of the æther in all directions. See PAM Dirac (24 November, 1951). "Is there an æther?". Nature vol 168: pp. 906-907.
4. ↑ Dirk Schwalm (2007). “The relativistic Doppler effect and time dilation”, Ewald Hiebl and Maurizio Musso, eds: Christian Doppler: life and work, principle and applications : proceedings of the Commemorative Symposia in 2003, Salzburg, Prague, Vienna, Venice. Living Edition, pp. 77 ff. ISBN 3901585095.
5. ↑ 5.0 5.1 Vidwan Singh Soni (2009). “§9.4.2: Transverse Doppler effect”, Mechanics and Relativity. PHI Learning Pvt. Ltd., pp. 306 ff. ISBN 8120337131.
6. ↑ For a discussion see Theo Koupelis (2010). “§4–7: The Doppler effect”, In Quest of the Universe, 6th ed. Jones & Bartlett Learning, pp. 115 ff. ISBN 0763768588.
7. ↑ For a discussion see Neil F. Comins, William J. Kaufmann (2008). “§6–12: The orbital motion of binary stars affects the wavelengths of their spectral lines”, Discovering the Universe: From the Stars to the Planets. Macmillan, pp. 174 ff. ISBN 1429230428.