# Gravitational redshift

The gravitational redshift of a light wave as it moves upwards against a gravitational field (produced by the yellow star below). The effect is greatly exaggerated in this diagram.

In astrophysics, gravitational redshift or Einstein shift is the process by which electromagnetic radiation originating from a source that is in a gravitational field is reduced in frequency, or redshifted, when observed in a region at a higher gravitational potential. This is a direct result of gravitational time dilation—if one is outside of an isolated gravitational source, the rate at which time passes increases as one moves away from that source. As frequency is inverse of time (specifically, time required for completing one wave oscillation), frequency of the electromagnetic radiation is reduced in an area of higher gravitational potential. There is a corresponding reduction in energy when electromagnetic radiation is red-shifted, as given by Planck's relation, due to the electromagnetic radiation propagating in opposition to the gravitational gradient. There also exists a corresponding blueshift when electromagnetic radiation propagates from an area of higher gravitational potential to an area of lower gravitational potential.

If applied to optical wavelengths, this manifests itself as a change in the colour of visible light as the wavelength of the light is shifted toward the red part of the light spectrum. Since frequency and wavelength are inversely proportional, this is equivalent to saying that the frequency of the light is reduced towards the red part of the light spectrum, giving this phenomenon the name redshift.

## DefinitionEdit

Redshift is often denoted with the dimensionless variable ${\displaystyle z\,}$ , defined as the fractional change of the wavelength[1]

${\displaystyle z={\frac {\lambda _{o}-\lambda _{e}}{\lambda _{e}}}}$

where ${\displaystyle \lambda _{o}\,}$  is the wavelength of the electromagnetic radiation (photon) as measured by the observer. ${\displaystyle \lambda _{e}\,}$  is the wavelength of the electromagnetic radiation (photon) when measured at the source of emission.

The gravitational redshift of a photon can be calculated in the framework of general relativity (using the Schwarzschild metric) as

${\displaystyle \lim _{r\to \infty }z(r)={\frac {1}{\sqrt {1-{\frac {r_{s}}{R_{e}}}}}}-1}$

${\displaystyle r_{s}={\frac {2GM}{c^{2}}}}$ ,

where ${\displaystyle G}$  denotes Newton's gravitational constant, ${\displaystyle M}$  the mass of the gravitating body, ${\displaystyle c}$  the speed of light, and ${\displaystyle R_{e}}$  the distance between the center of mass of the gravitating body and the point at which the photon is emitted. The redshift is not defined for photons emitted inside the Schwarzschild radius, the distance from the body where the escape velocity is greater than the speed of light. Therefore, this formula only applies when ${\displaystyle R_{e}}$  is larger than ${\displaystyle r_{s}}$ . When the photon is emitted at a distance equal to the Schwarzschild radius, the redshift will be infinitely large, and it will not escape to any finite distance from the Schwarzschild sphere. When the photon is emitted at an infinitely large distance, there is no redshift.

In the Newtonian limit, i.e. when ${\displaystyle R_{e}}$  is sufficiently large compared to the Schwarzschild radius ${\displaystyle r_{s}}$ , the redshift can be approximated by a binomial expansion to become

${\displaystyle \lim _{r\to \infty }z_{\mathrm {approx} }(r)={\frac {1}{2}}{\frac {r_{s}}{R_{e}}}={\frac {GM}{c^{2}R_{e}}}}$

The redshift formula for the frequency ${\displaystyle \nu =c/\lambda }$  (and therefore also for the energy ${\displaystyle h\nu }$  of a photon) can simply deduced from the wavelength-formula above to be

${\displaystyle \lim _{r\to \infty }\nu _{r}=\nu _{e}{\sqrt {1-{\frac {r_{s}}{R_{e}}}}}}$

with ${\displaystyle \nu _{e}}$  the emitted frequency at the emission point and ${\displaystyle \nu _{r}}$  the frequency at distance ${\displaystyle r>R_{e}}$  from the center of mass of the gravitating body causing this gravitational potential. Moreover, we get from the law of energy conservation ${\displaystyle h\nu _{\infty }=h\nu _{1}{\sqrt {1-{\frac {r_{s}}{R_{1}}}}}=h\nu _{2}{\sqrt {1-{\frac {r_{s}}{R_{2}}}}}}$  the general case for a photon of frequency ${\displaystyle \nu _{2}}$  emitted at distance ${\displaystyle R_{2}}$  to observer distance ${\displaystyle R_{1}}$  (measured as distances from the gravitational center of mass) the equation

${\displaystyle \nu _{1}=\nu _{2}{\sqrt {\frac {R_{1}(R_{2}-r_{s})}{R_{2}(R_{1}-r_{s})}}}}$

as long as ${\displaystyle R_{1},R_{2}>r_{s}}$  holds.

## HistoryEdit

The gravitational weakening of light from high-gravity stars was predicted by John Michell in 1783 and Pierre-Simon Laplace in 1796, using Isaac Newton's concept of light corpuscles (see: emission theory) and who predicted that some stars would have a gravity so strong that light would not be able to escape. The effect of gravity on light was then explored by Johann Georg von Soldner (1801), who calculated the amount of deflection of a light ray by the sun, arriving at the Newtonian answer which is half the value predicted by general relativity. All of this early work assumed that light could slow down and fall, which was inconsistent with the modern understanding of light waves.

Once it became accepted that light was an electromagnetic wave, it was clear that the frequency of light should not change from place to place, since waves from a source with a fixed frequency keep the same frequency everywhere. One way around this conclusion would be if time itself were altered—if clocks at different points had different rates.

This was precisely Einstein's conclusion in 1911. He considered an accelerating box, and noted that according to the special theory of relativity, the clock rate at the bottom of the box was slower than the clock rate at the top. Nowadays, this can be easily shown in accelerated coordinates. The metric tensor in units where the speed of light is one is:

${\displaystyle ds^{2}=-r^{2}dt^{2}+dr^{2}\,}$

and for an observer at a constant value of r, the rate at which a clock ticks, R(r), is the square root of the time coefficient, R(r)=r. The acceleration at position r is equal to the curvature of the hyperbola at fixed r, and like the curvature of the nested circles in polar coordinates, it is equal to 1/r.

So at a fixed value of g, the fractional rate of change of the clock-rate, the percentage change in the ticking at the top of an accelerating box vs at the bottom, is:

${\displaystyle {R(r+dr)-R(r) \over R}={dr \over r}=gdr\,}$

The rate is faster at larger values of R, away from the apparent direction of acceleration. The rate is zero at r=0, which is the location of the acceleration horizon.

Using the principle of equivalence, Einstein concluded that the same thing holds in any gravitational field, that the rate of clocks R at different heights was altered according to the gravitational field g. When g is slowly varying, it gives the fractional rate of change of the ticking rate. If the ticking rate is everywhere almost this same, the fractional rate of change is the same as the absolute rate of change, so that:

${\displaystyle {dR \over dx}=g=-{dV \over dx}\,}$

Since the rate of clocks and the gravitational potential have the same derivative, they are the same up to a constant. The constant is chosen to make the clock rate at infinity equal to 1. Since the gravitational potential is zero at infinity:

${\displaystyle R(x)=1-{V(x) \over c^{2}}\,}$

where the speed of light has been restored to make the gravitational potential dimensionless.

The coefficient of the ${\displaystyle dt^{2}}$  in the metric tensor is the square of the clock rate, which for small values of the potential is given by keeping only the linear term:

${\displaystyle R^{2}=1-2V\,}$

and the full metric tensor is:

${\displaystyle ds^{2}=-\left(1-{2V(r) \over c^{2}}\right)c^{2}dt^{2}+dx^{2}+dy^{2}+dz^{2}}$

where again the c's have been restored. This expression is correct in the full theory of general relativity, to lowest order in the gravitational field, and ignoring the variation of the space-space and space-time components of the metric tensor, which only affect fast moving objects.

Using this approximation, Einstein reproduced the incorrect Newtonian value for the deflection of light in 1909. But since a light beam is a fast moving object, the space-space components contribute too. After constructing the full theory of general relativity in 1916, Einstein solved for the space-space components in a post-Newtonian approximation, and calculated the correct amount of light deflection – double the Newtonian value. Einstein's prediction was confirmed by many experiments, starting with Arthur Eddington's 1919 solar eclipse expedition.

The changing rates of clocks allowed Einstein to conclude that light waves change frequency as they move, and the frequency/energy relationship for photons allowed him to see that this was best interpreted as the effect of the gravitational field on the mass–energy of the photon. To calculate the changes in frequency in a nearly static gravitational field, only the time component of the metric tensor is important, and the lowest order approximation is accurate enough for ordinary stars and planets, which are much bigger than their Schwarzschild radius.

## Important points to stressEdit

• The receiving end of the light transmission must be located at a higher gravitational potential in order for gravitational redshift to be observed. In other words, the observer must be standing "uphill" from the source. If the observer is at a lower gravitational potential than the source, a gravitational blueshift can be observed instead.
• Tests done by many universities continue to support the existence of gravitational redshift.[2]
• General relativity is not the only theory of gravity that predicts gravitational redshift. Other theories of gravitation require gravitational redshift, although their detailed explanations for why it appears vary.[citation needed] (Any theory that includes conservation of energy and mass–energy equivalence must include gravitational redshift.)
• Gravitational redshift does not assume the Schwarzschild metric solution to Einstein's field equation – in which the variable ${\displaystyle M\;}$  cannot represent the mass of any rotating or charged body.

## Experimental VerificationEdit

### Initial observations of gravitational redshift of white dwarf starsEdit

A number of experimenters initially claimed to have identified the effect using astronomical measurements, and the effect was considered to have been finally identified in the spectral lines of the star Sirius B by W.S. Adams in 1925.[3] However, measurements by Adams have been criticized as being too low[3][4] and these observations are now considered to be measurements of spectra that are unusable because of scattered light from the primary, Sirius B.[4] The first accurate measurement of the gravitational redshift of a white dwarf was done by Popper in 1954, measuring a 21 km/sec gravitational redshift of 40 Eridani B.[4]

The redshift of Sirius B was finally measured by Greenstein et al. in 1971, obtaining the value for the gravitational redshift of 89±19 km/sec, with more accurate measurements by the Hubble Space Telescope, showing 80.4±4.8 km/sec.

### Terrestrial testsEdit

The effect is now considered to have been definitively verified by the experiments of Pound, Rebka and Snider between 1959 and 1965. The Pound–Rebka experiment of 1959 measured the gravitational redshift in spectral lines using a terrestrial 57Fe gamma source over a vertical height of 22.5 metres.[5] using measurements of the change in wavelength of gamma-ray photons generated with the Mössbauer effect, which generates radiation with a very narrow line width. The accuracy of the gamma-ray measurements was typically 1%.

An improved experiment was done by Pound and Snider in 1965, with an accuracy better than the 1% level.[6]

A very accurate gravitational redshift experiment was performed in 1976,[7] where a hydrogen maser clock on a rocket was launched to a height of 10,000 km, and its rate compared with an identical clock on the ground. It tested the gravitational redshift to 0.007%.

Later tests can be done with the Global Positioning System (GPS), which must account for the gravitational redshift in its timing system, and physicists have analyzed timing data from the GPS to confirm other tests. When the first satellite was launched, it showed the predicted shift of 38 microseconds per day. This rate of discrepancy is sufficient to substantially impair function of GPS within hours if not accounted for. An excellent account of the role played by general relativity in the design of GPS can be found in Ashby 2003.

### Later Astronomical measurementsEdit

James W. Brault, a graduate student of Robert Dicke at Princeton University, measured the gravitational redshift of the sun using optical methods in 1962.

In 2011 the group of Radek Wojtak of the Niels Bohr Institute at the University of Copenhagen collected data from 8000 galaxy clusters and found that the light coming from the cluster centers tended to be red-shifted compared to the cluster edges, confirming the energy loss due to gravity.[8]

Other precision tests of general relativity,[9] not discussed here, are the Gravity Probe A satellite, launched in 1976, which showed gravity and velocity affect the ability to synchronize the rates of clocks orbiting a central mass; the Hafele–Keating experiment, which used atomic clocks in circumnavigating aircraft to test general relativity and special relativity together;[10][11] and the forthcoming Satellite Test of the Equivalence Principle.

## ApplicationEdit

Gravitational redshift is studied in many areas of astrophysical research.

## Exact SolutionsEdit

A table of exact solutions of the Einstein field equations consists of the following:

 Non-rotating Rotating Uncharged Schwarzschild Kerr Charged Reissner–Nordström Kerr–Newman

The more often used exact equation for gravitational redshift applies to the case outside of a non-rotating, uncharged mass which is spherically symmetric. The equation is:

${\displaystyle \lim _{r\to +\infty }z(r)={\frac {1}{\sqrt {1-\left({\frac {2GM}{R^{*}c^{2}}}\right)}}}-1}$ , where

• ${\displaystyle G\,}$  is the gravitational constant,
• ${\displaystyle M\,}$  is the mass of the object creating the gravitational field,
• ${\displaystyle R^{*}\,}$  is the radial coordinate of the point of emission (which is analogous to the classical distance from the center of the object, but is actually a Schwarzschild coordinate),
• ${\displaystyle r,}$  is the radial coordinate of the observer (in the formula, this observer is at an infinitely large distance), and
• ${\displaystyle c\,}$  is the speed of light.

## Gravitational redshift versus gravitational time dilationEdit

When using special relativity's relativistic Doppler relationships to calculate the change in energy and frequency (assuming no complicating route-dependent effects such as those caused by the frame-dragging of rotating black holes), then the gravitational redshift and blueshift frequency ratios are the inverse of each other, suggesting that the "seen" frequency-change corresponds to the actual difference in underlying clockrate. For rotating systems, route-dependence due to frame-dragging may complicate the process of determining globally-agreed differences in underlying clock rate.

While gravitational redshift refers to what is seen, gravitational time dilation refers to what is deduced to be "really" happening once observational effects are taken into account.

## NotesEdit

1. ^ See for example equation 29.3 of Gravitation by Misner, Thorne and Wheeler.
2. ^ General Relativity
3. ^ a b Hetherington, N. S., "Sirius B and the gravitational redshift - an historical review", Quarterly Journal Royal Astronomical Society, vol. 21, Sept. 1980, p. 246-252. Accessed 6 April 2017.
4. ^ a b c Holberg, J. B., "Sirius B and the Measurement of the Gravitational Redshift", Journal for the History of Astronomy, Vol. 41, 1, 2010, p. 41-64. Accessed 6 April 2017.
5. ^ Pound, R.; Rebka, G. (1960). "Apparent Weight of Photons". Physical Review Letters. 4 (7): 337–341. Bibcode:1960PhRvL...4..337P. doi:10.1103/PhysRevLett.4.337.. This paper was the first measurement.
6. ^ Pound, R. V.; Snider J. L. (November 2, 1964). "Effect of Gravity on Nuclear Resonance". Physical Review Letters. 13 (18): 539–540. Bibcode:1964PhRvL..13..539P. doi:10.1103/PhysRevLett.13.539.
7. ^ Vessot, R. F. C.; M. W. Levine; E. M. Mattison; E. L. Blomberg; T. E. Hoffman; G. U. Nystrom; B. F. Farrel; R. Decher; et al. (December 29, 1980). "Test of Relativistic Gravitation with a Space-Borne Hydrogen Maser". Physical Review Letters. 45 (26): 2081–2084. Bibcode:1980PhRvL..45.2081V. doi:10.1103/PhysRevLett.45.2081.
8. ^ Bhattacharjee, Yudhijit (2011). "Galaxy Clusters Validate Einstein's Theory". News.sciencemag.org. Retrieved 2013-07-23.
9. ^ "Gravitational Physics with Optical Clocks in Space" (PDF). S. Schiller (PDF). Heinrich Heine Universität Düsseldorf. 2007. Retrieved 19 March 2015.
10. ^ Hafele, J. C.; Keating, R. E. (July 14, 1972). "Around-the-World Atomic Clocks: Predicted Relativistic Time Gains". Science. 177 (4044): 166–168. Bibcode:1972Sci...177..166H. doi:10.1126/science.177.4044.166. PMID 17779917.
11. ^ Hafele, J. C.; Keating, R. E. (July 14, 1972). "Around-the-World Atomic Clocks: Observed Relativistic Time Gains". Science. 177 (4044): 168–170. Bibcode:1972Sci...177..168H. doi:10.1126/science.177.4044.168. PMID 17779918.

## Primary sourcesEdit

• Michell, John (1784). "On the means of discovering the distance, magnitude etc. of the fixed stars". Philosophical Transactions of the Royal Society. 74: 35–57. doi:10.1098/rstl.1784.0008.