Uniform gravitational field or acceleration

Einstein's theory of general relativity incorporates the equivalence principle, which can be stated in various different ways. One such statement is that gravitational effects are locally undetectable for a free-falling observer. Therefore, in a laboratory experiment at the surface of the Earth, all gravitational effects should be equivalent to the effects that would have been observed if the laboratory had been accelerating through outer space at g. One consequence is a gravitational Doppler effect. If a light pulse is emitted at the floor of the laboratory, then a free-falling observer says that by the time it reaches the ceiling, the ceiling has accelerated away from it, and therefore when observed by a detector fixed to the ceiling, it will be observed to have been Doppler shifted toward the red end of the spectrum. This shift, which the free-falling observer considers to be a kinematical Doppler shift, is thought of by the laboratory observer as a gravitational redshift. Such an effect was verified in the 1959 Pound–Rebka experiment. In a case such as this, where the gravitational field is uniform, the change in wavelength is given by

${\displaystyle z={\frac {\Delta \lambda }{\lambda }}\approx {\frac {g\Delta y}{c^{2}}},}$

where ${\displaystyle \Delta y}$ is the change in height. Since this prediction arises directly from the equivalence principle, it does not require any of the mathematical apparatus of general relativity, and its verification does not specifically support general relativity over any other theory that incorporates the equivalence principle.

On Earth's surface (or in a spaceship accelerating at 1 g), the gravitational redshift is approximately 1.1 × 10⁻¹⁶, the equivalent of a 3.3 × 10⁻⁸ m/s Doppler shift, for every meter of height differential.

Spherically symmetric gravitational field

When the field is not uniform, the simplest and most useful case to consider is that of a spherically symmetric field. By Birkhoff's theorem, such a field is described in general relativity by the Schwarzschild metric, ${\displaystyle d\tau ^{2}=\left(1-r_{\text{S}}/R\right)dt^{2}+\ldots }$, where ${\displaystyle d\tau }$ is the clock time of an observer at distance R from the center, ${\displaystyle dt}$ is the time measured by an observer at infinity, ${\displaystyle r_{\text{S}}}$ is the Schwarzschild radius ${\displaystyle 2GM/c^{2}}$, "..." represents terms that vanish if the observer is at rest, ${\displaystyle G}$ is Newton's gravitational constant, ${\displaystyle M}$ the mass of the gravitating body, and ${\displaystyle c}$ the speed of light. The result is that frequencies and wavelengths are shifted according to the ratio

${\displaystyle 1+z={\frac {\lambda _{\infty }}{\lambda _{\text{e}}}}=\left(1-{\frac {r_{\text{S}}}{R_{\text{e}}}}\right)^{-{\frac {1}{2}}}}$

where

• ${\displaystyle \lambda _{\infty }\,}$is the wavelength of the light as measured by the observer at infinity,
• ${\displaystyle \lambda _{\text{e}}\,}$ is the wavelength measured at the source of emission, and
• ${\displaystyle R_{\text{e}}}$ is the radius at which the photon is emitted.

This can be related to the redshift parameter conventionally defined as ${\displaystyle z=\lambda _{\infty }/\lambda _{\text{e}}-1}$.

In the case where neither the emitter nor the observer is at infinity, the transitivity of Doppler shifts allows us to generalize the result to ${\displaystyle \lambda _{1}/\lambda _{2}=\left[\left(1-r_{\text{S}}/R_{1}\right)/\left(1-r_{\text{S}}/R_{2}\right)\right]^{1/2}}$. The redshift formula for the frequency ${\displaystyle \nu =c/\lambda }$ is ${\displaystyle \nu _{o}/\nu _{\text{e}}=\lambda _{\text{e}}/\lambda _{o}}$. When ${\displaystyle R_{1}-R_{2}}$ is small, these results are consistent with the equation given above based on the equivalence principle.

The redshift ratio may also be expressed in terms of a (Newtonian) escape velocity ${\displaystyle v_{\text{e}}}$ at ${\displaystyle R_{\text{e}}=2GM/v_{\text{e}}^{2}}$, resulting in the corresponding Lorentz factor:

${\displaystyle 1+z=\gamma _{\text{e}}={\frac {1}{\sqrt {1-(v_{\text{e}}/c)^{2}}}}}$.

For an object compact enough to have an event horizon, the redshift is not defined for photons emitted inside the Schwarzschild radius, both because signals cannot escape from inside the horizon and because an object such as the emitter cannot be stationary inside the horizon, as was assumed above. Therefore, this formula only applies when ${\displaystyle R_{\text{e}}}$ is larger than ${\displaystyle r_{\text{S}}}$. 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.

Astronomical observations

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.^[14] However, measurements by Adams have been criticized as being too low^[14][15] and these observations are now considered to be measurements of spectra that are unusable because of scattered light from the primary, Sirius A.^[15] The first accurate measurement of the gravitational redshift of a white dwarf was done by Popper in 1954, measuring a 21 km/s gravitational redshift of 40 Eridani B.^[15] The redshift of Sirius B was finally measured by Greenstein et al. in 1971, obtaining the value for the gravitational redshift of 89±16 km/s, with more accurate measurements by the Hubble Space Telescope, showing 80.4±4.8 km/s.^[16]

James W. Brault, a graduate student of Robert Dicke at Princeton University, measured the gravitational redshift of the sun using optical methods in 1962.^[17] In 2020, a team of scientists published the most accurate measurement of the solar gravitational redshift so far, made by analyzing Fe spectral lines in sunlight reflected by the Moon; their measurement of a mean global 638 ± 6 m/s lineshift is in agreement with the theoretical value of 633.1 m/s.^[18][19] Measuring the solar redshift is complicated by the Doppler shift caused by the motion of the Sun's surface, which is of similar magnitude as the gravitational effect.^[19]

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.^[20]

In 2018, the star S2 made its closest approach to Sgr A*, the 4-million solar mass supermassive black hole at the centre of the Milky Way, reaching 7650 km/s or about 2.5% of the speed of light while passing the black hole at a distance of just 120 AU, or 1400 Schwarzschild radii. Independent analyses by the GRAVITY collaboration^{[21][22][23][24]} (led by Reinhard Genzel) and the KECK/UCLA Galactic Center Group^[25][26] (led by Andrea Ghez) revealed a combined transverse Doppler and gravitational redshift up to 200 km/s/c, in agreement with general relativity predictions.

In 2021, Mediavilla (IAC, Spain) & Jiménez-Vicente (UGR, Spain) were able to use measurements of the gravitational redshift in quasars up to cosmological redshift of z~3 to confirm the predictions of Einstein's Equivalence Principle and the lack of cosmological evolution within 13%.^[27]

Terrestrial tests

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.^[28] This paper was the first determination of the gravitational redshift which used 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.^[29]

A very accurate gravitational redshift experiment was performed in 1976,^[30] 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 the discrepancy is sufficient to substantially impair the 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.^[31]

In 2010, an experiment placed two aluminum-ion quantum clocks close to each other, but with the second elevated 33 cm compared to the first, making the gravitational red shift effect visible in everyday lab scales.^[32][33]

In 2020, a group at the University of Tokyo measured the gravitational redshift of two strontium-87 optical lattice clocks.^[34] The measurement took place at Tokyo Tower where the clocks were separated by approximately 450 m and connected by telecom fibers. The gravitational redshift can be expressed as

${\displaystyle z={\frac {\Delta \nu }{\nu _{1}}}=(1+\alpha ){\frac {\Delta U}{c^{2}}}}$,

where ${\displaystyle \Delta \nu =\nu _{2}-\nu _{1}}$ is the gravitational redshift, ${\displaystyle \nu _{1}}$ is the optical clock transition frequency, ${\displaystyle \Delta U=U_{2}-U_{1}}$ is the difference in gravitational potential, and ${\displaystyle \alpha }$ denotes the violation from general relativity. By Ramsey spectroscopy of the strontium-87 optical clock transition (429 THz, 698 nm) the group determined the gravitational redshift between the two optical clocks to be 21.18 Hz, corresponding to a z-value of approximately 5 × 10⁻¹⁴. Their measured value of ${\displaystyle \alpha }$, ${\displaystyle (1.4\pm 9.1)\times 10^{-5}}$, is an agreement with recent measurements made with hydrogen masers in elliptical orbits.^[35][36]

In October 2021, a group at JILA led by physicist Jun Ye reported a measurement of gravitational redshift in the submillimeter scale. The measurement is done on the ⁸⁷Sr clock transition between the top and the bottom of a millimeter-tall ultracold cloud of 100,000 strontium atoms in an optical lattice.^[37][38]

Primary sources

• 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. Bibcode:1784RSPT...74...35M. doi:10.1098/rstl.1784.0008.
• Laplace, Pierre-Simon (1796). The system of the world. Vol. 2 (1809 English translation ed.). London: Richard Phillips. pp. 366–368.
• von Soldner, Johann Georg (1804). "On the deflection of a light ray from its rectilinear motion, by the attraction of a celestial body at which it nearly passes by" . Berliner Astronomisches Jahrbuch: 161–172.
• Albert Einstein, "Relativity: the Special and General Theory". (@Project Gutenberg).
• Pound, R.V.; Rebka, G.A. Jr. (1959). "Gravitational Red-Shift in Nuclear Resonance". Phys. Rev. Lett. 3 (9): 439–441. Bibcode:1959PhRvL...3..439P. doi:10.1103/physrevlett.3.439.
• Pound, R.V.; Snider, J.L. (1965). "Effect of gravity on gamma radiation". Phys. Rev. B. 140 (3B): 788–803. Bibcode:1965PhRv..140..788P. doi:10.1103/physrev.140.b788.
• Pound, R.V. (2000). "Weighing Photons" (2000)". Classical and Quantum Gravity. 17 (12): 2303–2311. Bibcode:2000CQGra..17.2303P. doi:10.1088/0264-9381/17/12/301. S2CID 250886562.

Other sources

• Misner, Charles W.; Thorne, Kip S.; Wheeler, John Archibald (1973-09-15). Gravitation. San Francisco: W. H. Freeman. ISBN 978-0-7167-0344-0.