Although it is possible to reflect light or radio waves directly from the Moon's surface (a process known as
EME), a much more precise range measurement can be made using retroreflectors, since because of their small size, the temporal spread in the reflected signal is much smaller.[4]
The uncrewed Soviet Lunokhod 1 and Lunokhod 2 rovers carried smaller arrays. Reflected signals were initially received from Lunokhod 1 by the Soviet Union up to 1974, but not by western observatories that did not have precise information about location. In 2010
NASA's
Lunar Reconnaissance Orbiter located the Lunokhod 1 rover on images and in April 2010 a team from University of California ranged the array.[10]Lunokhod 2's array continues to return signals to Earth.[11] The Lunokhod arrays suffer from decreased performance in direct sunlight—a factor considered in reflector placement during the Apollo missions.[12]
The Apollo 15 array is three times the size of the arrays left by the two earlier Apollo missions. Its size made it the target of three-quarters of the sample measurements taken in the first 25 years of the experiment. Improvements in technology since then have resulted in greater use of the smaller arrays, by sites such as the
Côte d'Azur Observatory in
Nice, France; and the
Apache Point Observatory Lunar Laser-ranging Operation (APOLLO) at the
Apache Point Observatory in
New Mexico.
In the 2010s several
new retroreflectors were planned. The
MoonLIGHT reflector, which was to be placed by the private
MX-1E lander, was designed to increase measurement accuracy up to 100 times over existing systems.[13][14][15] MX-1E was set to launch in July 2020,[16] however, as of February 2020, the launch of the MX-1E has been canceled.[17] India's
Chandrayaan-3 lunar lander successfully placed a sixth reflector on the Moon in August 2023.[3] MoonLIGHT will be launched in early 2024 with a
Commercial Lunar Payload Services (CLPS) mission.[18]
The distance to the Moon is calculated approximately using the equation:
distance = (speed of light × duration of delay due to reflection) / 2. Since the
speed of light is a defined constant, conversion between distance and time of flight can be made without ambiguity.
To compute the lunar distance precisely, many factors must be considered in addition to the round-trip time of about 2.5 seconds. These factors include the location of the Moon in the sky, the relative motion of Earth and the Moon, Earth's rotation,
lunar libration,
polar motion,
weather, speed of light in various parts of air, propagation delay through
Earth's atmosphere, the location of the observing station and its motion due to
crustal motion and
tides, and
relativistic effects.[20][21] The distance continually changes for a number of reasons, but averages 385,000.6 km (239,228.3 mi) between the center of the Earth and the center of the Moon.[22] The orbits of the Moon and planets are integrated numerically along with the orientation of the Moon called physical
libration.[23]
At the Moon's surface, the beam is about 6.5 kilometers (4.0 mi) wide[24][i] and scientists liken the task of aiming the beam to using a rifle to hit a moving
dime 3 kilometers (1.9 mi) away. The reflected light is too weak to see with the human eye. Out of a pulse of 3×1017 photons[25] aimed at the reflector, only about 1–5 are received back on Earth, even under good conditions.[26] They can be identified as originating from the laser because the laser is highly
monochromatic.
As of 2009, the distance to the Moon can be measured with millimeter precision.[27] In a relative sense, this is one of the most precise distance measurements ever made, and is equivalent in accuracy to determining the distance between Los Angeles and New York to within the width of a human hair.
The Lunar Laser Ranging data is collected in order to extract numerical values for a number of parameters. Analyzing the range data involves dynamics, terrestrial geophysics, and lunar geophysics. The modeling problem involves two aspects: an accurate computation of the lunar orbit and lunar orientation, and an accurate model for the time of flight from an observing station to a retroreflector and back to the station. Modern Lunar Laser Ranging data can be fit with a 1 cm weighted rms residual.
The center of Earth to center of Moon distance is computed by a program that numerically integrates the lunar and planetary orbits accounting for the gravitational attraction of the Sun, planets, and a selection of asteroids.[36][23]
The same program integrates the 3-axis orientation of the Moon called physical
Libration.
Tides in the solid Earth and seasonal motion of the solid Earth with respect to its center of mass.
Relativistic transformation of time and space coordinates from a frame moving with the station to a frame fixed with respect to the solar system center of mass. Lorentz contraction of the Earth is part of this transformation.
Delay in the Earth's atmosphere.
Relativistic delay due to the gravity fields of the Sun, Earth, and Moon.
The position of the retroreflector accounting for orientation of the Moon and solid-body tides.
Lorentz contraction of the Moon.
Thermal expansion and contraction of the retroreflector mounts.
For the terrestrial model, the IERS Conventions (2010) is a source of detailed information.[38]
Results
Lunar laser ranging measurement data is available from the Paris Observatory Lunar Analysis Center,[39] the International Laser Ranging Service archives,[40][41] and the active stations. Some of the findings of this
long-term experiment are:[22]
Properties of the Moon
The distance to the Moon can be measured with millimeter precision.[27]
The Moon is spiraling away from Earth at a rate of 3.8 cm/year.[24][42] This rate has been described as anomalously high.[43]
The fluid core of the Moon was detected from the effects of core/mantle boundary dissipation.[44]
The Moon has free physical
librations that require one or more stimulating mechanisms.[45]
Tidal dissipation in the Moon depends on tidal frequency.[42]
The Moon probably has a liquid core of about 20% of the Moon's radius.[11] The radius of the lunar core-mantle boundary is determined as 381±12 km.[46]
The polar
flattening of the lunar core-mantle boundary is determined as (2.2±0.6)×10−4.[46]
The free core
nutation of the Moon is determined as 367±100 yr.[46]
Accurate locations for retroreflectors serve as reference points visible to orbiting spacecraft.[47]
Gauge freedom plays a major role in a correct physical interpretation of the relativistic effects in the Earth-Moon system observed with LLR technique.[49]
The likelihood of any
Nordtvedt effect (a hypothetical differential acceleration of the Moon and Earth towards the Sun caused by their different degrees of compactness) has been ruled out to high precision,[50][48][51] strongly supporting the
strong equivalence principle.
The universal force of
gravity is very stable. The experiments have constrained the change in
Newton'sgravitational constantG to a factor of (2±7)×10−13 per year.[52]
^During the round-trip time, an Earth observer will have moved by around 1 km (depending on their latitude). This has been presented, incorrectly, as a 'disproof' of the ranging experiment, the claim being that the beam to such a small reflector cannot hit such a moving target. However the size of the beam is far larger than any movement, especially for the returned beam.
^Chapront, J.; Chapront-Touzé, M.; Francou, G. (1999). "Determination of the lunar orbital and rotational parameters and of the ecliptic reference system orientation from LLR measurements and IERS data". Astronomy and Astrophysics. 343: 624–633.
Bibcode:
1999A&A...343..624C.
^
abcWilliams, James G.; Dickey, Jean O. (2002).
Lunar Geophysics, Geodesy, and Dynamics(PDF). 13th International Workshop on Laser Ranging. 7–11 October 2002. Washington, D. C.
^Viswanathan, V; Fienga, A; Minazzoli, O; Bernus, L; Laskar, J; Gastineau, M (May 2018). "The new lunar ephemeris INPOP17a and its application to fundamental physics". Monthly Notices of the Royal Astronomical Society. 476 (2): 1877–1888.
arXiv:1710.09167.
Bibcode:
2018MNRAS.476.1877V.
doi:
10.1093/mnras/sty096.