Shapiro delay

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The Shapiro time delay effect, or gravitational time delay effect, is one of the four classic solar system tests of general relativity. Radar signals passing near a massive object take slightly longer to travel to a target and longer to return than they would if the mass of the object were not present. The time delay is caused by the slowing of light as it moves through a change in gravitational potential. In an article entitled Fourth Test of General Relativity, Shapiro et al. wrote [1]

The proposed experiment was designed to verify the prediction that the speed of propagation of a light ray decreases as it passes through a region of decreasing gravitational potential

History[edit]

The time delay effect was first noticed in 1964, by Irwin Shapiro. Shapiro proposed an observational test of his prediction: bounce radar beams off the surface of Venus and Mercury, and measure the round trip travel time. When the Earth, Sun, and Venus are most favorably aligned, Shapiro showed that the expected time delay, due to the presence of the Sun, of a radar signal traveling from the Earth to Venus and back, would be about 200 microseconds,[2] well within the limitations of 1960s era technology.

The first tests, performed in 1966 and 1967 using the MIT Haystack radar antenna, were successful, matching the predicted amount of time delay.[3] The experiments have been repeated many times since then, with increasing accuracy.

Calculating time delay[edit]

In a near-static gravitational field of moderate strength (say, of stars and planets, but not one of a black hole or close binary system of neutron stars) the effect may be considered as a special case of gravitational time dilation.The measured elapsed time of a light signal in a gravitational field is longer than it would be without the field, and for moderate strength near-static fields the difference is directly proportional to the classical gravitational potential, precisely as given by standard gravitational time dilation formulas.

Time delay due to light traveling around a single mass[edit]

For a signal going around a massive object, the time delay can be calculated as the following:

\Delta t=-\frac{2GM}{c^3}\log(1-\mathbf{R}\cdot\mathbf{x})

Here R is the unit vector pointing from the observer to the source, and x is the unit vector pointing from the observer to the gravitating mass M. The dot denotes the usual Euclidean dot product.

Using Δx = cΔt, this formula can also be written as

\Delta x= -R_s \log(1-\mathbf{R}\cdot\mathbf{x}),

which is the extra distance the light has to travel. Here R_s is the Schwarzschild radius.

In PPN parameters,

\Delta t = -(1+\gamma)\frac{R_s}{2c} \log(1-\mathbf{R}\cdot\mathbf{x}),

which is twice the Newtonian prediction (with \gamma = 0).[4]

Interplanetary probes[edit]

Shapiro delay must be considered along with ranging data when trying to accurately determine the distance to interplanetary probes such as the Voyager and Pioneer spacecraft.

Shapiro delay of neutrinos and gravitational waves[edit]

From the near-simultaneous observations of neutrinos and photons from SN 1987A, the Shapiro delay for high-energy neutrinos must be the same as that for photons to within 10%, consistent with recent estimates of the neutrino mass which imply that those neutrinos were moving at very close to the speed of light. Since gravitational waves have not been directly detected, there is no data on the Shapiro delay for gravitational waves. In general relativity and other metric theories of gravity, though, the Shapiro delay for gravitational waves is expected to be the same as that for light and neutrinos. However, in theories such as tensor-vector-scalar gravity and other modified GR theories which reproduce Milgrom's law and avoid the need for dark matter, the Shapiro delay for gravitational waves is much smaller than that for neutrinos or photons.

See also[edit]

References[edit]

  1. ^ Irwin I. Shapiro (1964). "Fourth Test of General Relativity". Physical Review Letters 13 (26): 789–791. Bibcode:1964PhRvL..13..789S. doi:10.1103/PhysRevLett.13.789. 
  2. ^ Irwin I. Shapiro (1964). "Fourth Test of General Relativity". Physical Review Letters 13 (26): 789–791. Bibcode:1964PhRvL..13..789S. doi:10.1103/PhysRevLett.13.789. 
  3. ^ Irwin I. Shapiro, Gordon H. Pettengill, Michael E. Ash, Melvin L. Stone, William B. Smith, Richard P. Ingalls, and Richard A. Brockelman (1968). "Fourth Test of General Relativity: Preliminary Results". Physical Review Letters 20 (22): 1265–1269. Bibcode:1968PhRvL..20.1265S. doi:10.1103/PhysRevLett.20.1265. 
  4. ^ Elena V. Pitjeva: Tests of General Relativity from observations of planets and spacecraft - [1]

Further reading[edit]