Jump to content

Lunar distance

From Wikipedia, the free encyclopedia
(Redirected from Lunar distances)
For the navigation unit, see Lunar distance (navigation).
Lunar distance
A lunar distance, 384,399 km (238,854 mi), is the Moon's average distance to Earth. The actual distance varies over the course of its orbit. The image compares the Moon's apparent size when it is nearest and farthest from Earth.
General information
Unit systemastronomy
Unit ofdistance
SymbolLD, 
Conversions
1 LD in ...... is equal to ...
   SI base unit   3.84399×108 m
   Metric system   384399 km
   English units   238854 miles
   Astronomical unit   0.002569 au
   Lightsecond   1.28 ls

The instantaneous Earth–Moon distance, or distance to the Moon, is the distance from the center of Earth to the center of the Moon. In contrast, the Lunar distance (LD or ), or Earth–Moon characteristic distance, is a unit of measure in astronomy. More technically, it is the semi-major axis of the geocentric lunar orbit. The lunar distance is on average approximately 385,000 km (239,000 mi), or 1.28 light-seconds; this is roughly 30 times Earth's diameter or 9.5 times Earth's circumference. Around 389 lunar distances make up an AU astronomical unit (roughly the distance from Earth to the Sun).

Lunar distance is commonly used to express the distance to near-Earth object encounters.[1] Lunar semi-major axis is an important astronomical datum; the few-millimeter precision of the range measurements determines semi-major axis to a few decimeters; it has implications for testing gravitational theories such as general relativity and [2] and for refining other astronomical values, such as the mass,[3] radius,[4] and rotation of Earth.[5] The measurement is also useful in expressing the lunar radius, as well as the distance to the Sun.

Millimeter-precision measurements of the lunar distance are made by measuring the time taken for laser beam light to travel between stations on Earth and retroreflectors placed on the Moon. The Moon is spiraling away from Earth at an average rate of 3.8 cm (1.5 in) per year, as detected by the Lunar Laser Ranging experiment.[6][7][8]

Value

[edit]
Variation of the distance between the centers of the Moon and the Earth over 700 days.
Distribution of perigee and apogee between 3000 BC and AD 3000.

Because of the influence of the Sun and other perturbations, the Moon's orbit around the Earth is not a precise ellipse. Nevertheless, different methods have been used to define a semi-major axis. Ernest William Brown provided a formula for the parallax of the Moon as viewed from opposite sides of the Earth, involving trigonometric terms. This is equivalent to a formula for the inverse of the distance, and the average value of this is the inverse of 384,399 km (238,854 mi).[9][10] On the other hand, the time-averaged distance (rather than the inverse of the average inverse distance) between the centers of Earth and the Moon is 385,000.6 km (239,228.3 mi). One can also model the orbit as an ellipse that is constantly changing, and in this case one can find a formula for the semi-major axis, again involving trigonometric terms. The average value by this method is 383,397 km.[11]

The actual distance varies over the course of the orbit of the Moon. Values at closest approach (perigee) or at farthest (apogee) are rarer the more extreme they are. The graph at right shows the distribution of perigee and apogee over six thousand years.

Jean Meeus gives the following extreme values for 1500 BC to AD 8000:[12]

  • greatest distance: 406 719.97 km on January 7, AD 2266
  • smallest distance: 356 352.93 km on November 13, 1054 BC
Lunar distance expressed in selected units
Unit Mean value Uncertainty
meter 3.84399×108 1.1 mm[13]
kilometer 384,399 1.1 mm[13]
mile 238,854 0.043 in[13]
Earth radius 60.32[14]
AU ⁠1/388.6⁠ = 0.00257

[15][16]

light-second 1.282 37.5×10−12[13]
  • An AU is 389 Lunar distances.[17]
  • A lightyear is 24,611,700 Lunar distances.[17][18]
  • Geostationary Earth Orbit is 42,164 km (26,199 mi) from Earth center, or ⁠1/9.117⁠ LD = 0.10968 LD (or 0.10968 LDEO[19])
Distance between the Earth and Moon (mean value) – sizes and distance to scale – with travel time at speed of light animated
Photo of Earth and Moon, taken by the OSIRIS-REx probe
Lunar distance to scale, with Medium Earth orbital (MEO) space as pink area for reference.

Variation

[edit]

The instantaneous lunar distance is constantly changing. The actual distance between the Moon and Earth can change as quickly as 75 meters per second,[20] or more than 1,000 km (620 mi) in just 6 hours, due to its non-circular orbit.[21] There are other effects that also influence the lunar distance. Some factors include:

Minimum, mean and maximum distances of the Moon from Earth with its angular diameter as seen from Earth's surface, to scale
Lunar distance when perigee is at syzygy (full moon or new moon, in blue) or at half moon (red). The horizontal lines (extending exactly half a mean anomalistic month to each side of perigee) are the respective averages over one mean anomalistic month, and are almost identical.

The formula of Chapront and Touzé for the distance in kilometres begins with the terms:[9]

where is the mean anomaly (more or less how moon has moved from perigee) and is the mean elongation (more or less how far it has moved from conjunction with the Sun at new moon). They can be calculated from

GM = 134.963 411 38° + 13.064 992 953 630°/d · t

D = 297.850 204 20° + 12.190 749 117 502°/d · t

where t is the time (in days) since January 1, 2000 (see Epoch (astronomy)). This shows that the smallest perigee occurs at either new moon or full moon (ca 356870 km), as does the greatest apogee (ca 406079 km), whereas the greatest perigee will be around half-moon (ca 370180 km), as will be the smallest apogee (ca 404593 km). The exact values will be slightly different due to other terms. Twice in every full moon cycle of about 411 days there will be a minimal perigee and a maximal apogee, separated by two weeks, and a maximal perigee and a minimal apogee, also separated by two weeks.

Perturbations and eccentricity

[edit]

The distance to the Moon can be measured to an accuracy of 2 mm over a 1-hour sampling period,[22] which results in an overall uncertainty of a decimeter for the semi-major axis. However, due to its elliptical orbit with varying eccentricity, the instantaneous distance varies with monthly periodicity. Furthermore, the distance is perturbed by the gravitational effects of various astronomical bodies – most significantly the Sun and less so Venus and Jupiter. Other forces responsible for minute perturbations are: gravitational attraction to other planets in the Solar System and to asteroids; tidal forces; and relativistic effects.[23][24] The effect of radiation pressure from the Sun contributes an amount of ±3.6 mm to the lunar distance.[22]

Although the instantaneous uncertainty is a few millimeters, the measured lunar distance can change by more than 30,000 km (19,000 mi) from the mean value throughout a typical month. These perturbations are well understood[25] and the lunar distance can be accurately modeled over thousands of years.[23]

The Moon's distance from the Earth and Moon phases in 2014.
Moon phases: 0 (1) – new moon, 0.25 – first quarter, 0.5 – full moon, 0.75 – last quarter.

Tidal dissipation

[edit]

Through the action of tidal forces, the angular momentum of Earth's rotation is slowly being transferred to the Moon's orbit.[26] The result is that Earth's rate of spin is gradually decreasing (at a rate of 2.4 milliseconds/century),[27][28][29][30] and the lunar orbit is gradually expanding. The rate of recession is 3.830±0.008 cm per year.[25][28] However, it is believed that this rate has recently increased, as a rate of 3.8 cm/year would imply that the Moon is only 1.5 billion years old, whereas scientific consensus supports an age of about 4 billion years.[31] It is also believed that this anomalously high rate of recession may continue to accelerate.[32]

Theoretically, the lunar distance will continue to increase until the Earth and Moon become tidally locked, as are Pluto and Charon. This would occur when the duration of the lunar orbital period equals the rotational period of Earth, which is estimated to be 47 Earth days. The two bodies would then be at equilibrium, and no further rotational energy would be exchanged. However, models predict that 50 billion years would be required to achieve this configuration,[33] which is significantly longer than the expected lifetime of the Solar System.

Orbital history

[edit]

Laser measurements show that the average lunar distance is increasing, which implies that the Moon was closer in the past, and that Earth's days were shorter. Fossil studies of mollusk shells from the Campanian era (80 million years ago) show that there were 372 days (of 23 h 33 min) per year during that time, which implies that the lunar distance was about 60.05 R🜨 (383,000 km or 238,000 mi).[26] There is geological evidence that the average lunar distance was about 52 R🜨 (332,000 km or 205,000 mi) during the Precambrian Era; 2500 million years BP.[31]

The widely accepted giant impact hypothesis states that the Moon was created as a result of a catastrophic impact between Earth and another planet, resulting in a re-accumulation of fragments at an initial distance of 3.8 R🜨 (24,000 km or 15,000 mi).[34] This theory assumes the initial impact to have occurred 4.5 billion years ago.[35]

History of measurement

[edit]

Until the late 1950s all measurements of lunar distance were based on optical angular measurements: the earliest accurate measurement was by Hipparchus in the 2nd century BC. The space age marked a turning point when the precision of this value was much improved. During the 1950s and 1960s, there were experiments using radar, lasers, and spacecraft, conducted with the benefit of computer processing and modeling.[36]

Some historically significant or otherwise interesting methods of determining the lunar distance:

Parallax

[edit]

The oldest method of determining the lunar distance involved measuring the angle between the Moon and a chosen reference point from multiple locations, simultaneously. The synchronization can be coordinated by making measurements at a pre-determined time, or during an event which is observable to all parties. Before accurate mechanical chronometers, the synchronization event was typically a lunar eclipse, or the moment when the Moon crossed the meridian (if the observers shared the same longitude). This measurement technique is known as lunar parallax.

For increased accuracy, the measured angle can be adjusted to account for refraction and distortion of light passing through the atmosphere.

Lunar eclipse

[edit]

Early attempts to measure the distance to the Moon exploited observations of a lunar eclipse combined with knowledge of Earth's radius and an understanding that the Sun is much further than the Moon. By observing the geometry of a lunar eclipse, the lunar distance can be calculated using trigonometry.

The earliest accounts of attempts to measure the lunar distance using this technique were by Greek astronomer and mathematician Aristarchus of Samos in the 4th century BC[37] and later by Hipparchus, whose calculations produced a result of 59–67 R🜨 (376000–427000 km or 233000–265000 mi).[38] This method later found its way into the work of Ptolemy,[39] who produced a result of 64+1⁄6 R🜨 (409000 km or 253000 mi) at its farthest point.[40]

Meridian crossing

[edit]

An expedition by French astronomer A.C.D. Crommelin observed lunar meridian transits on the same night from two different locations. Careful measurements from 1905 to 1910 measured the angle of elevation at the moment when a specific lunar crater (Mösting A) crossed the local meridian, from stations at Greenwich and at Cape of Good Hope.[41] A distance was calculated with an uncertainty of 30 km, and this remained the definitive lunar distance value for the next half century.

Occultations

[edit]

By recording the instant when the Moon occults a background star, (or similarly, measuring the angle between the Moon and a background star at a predetermined moment) the lunar distance can be determined, as long as the measurements are taken from multiple locations of known separation.

Astronomers O'Keefe and Anderson calculated the lunar distance by observing four occultations from nine locations in 1952.[42] They calculated a semi-major axis of 384407.6±4.7 km (238,859.8 ± 2.9 mi). This value was refined in 1962 by Irene Fischer, who incorporated updated geodetic data to produce a value of 384403.7±2 km (238,857.4 ± 1 mi).[4]

Radar

[edit]
Oscilloscope display showing the radar signal.[43] The large pulse on the left is the transmitted signal, the small pulse on the right is the return signal from the Moon. The horizontal axis is time, but is calibrated in miles. It can be seen that the measured range is 238,000 mi (383,000 km), approximately the distance from the Earth to the Moon

The distance to the moon was measured by means of radar first in 1946 as part of Project Diana.[44]

Later, an experiment was conducted in 1957 at the U.S. Naval Research Laboratory that used the echo from radar signals to determine the Earth-Moon distance. Radar pulses lasting 2 μs were broadcast from a 50-foot (15 m) diameter radio dish. After the radio waves echoed off the surface of the Moon, the return signal was detected and the delay time measured. From that measurement, the distance could be calculated. In practice, however, the signal-to-noise ratio was so low that an accurate measurement could not be reliably produced.[45]

The experiment was repeated in 1958 at the Royal Radar Establishment, in England. Radar pulses lasting 5 μs were transmitted with a peak power of 2 megawatts, at a repetition rate of 260 pulses per second. After the radio waves echoed off the surface of the Moon, the return signal was detected and the delay time measured. Multiple signals were added together to obtain a reliable signal by superimposing oscilloscope traces onto photographic film. From the measurements, the distance was calculated with an uncertainty of 1.25 km (0.777 mi).[46]

These initial experiments were intended to be proof-of-concept experiments and only lasted one day. Follow-on experiments lasting one month produced a semi-major axis of 384402±1.2 km (238,856 ± 0.75 mi),[47] which was the most precise measurement of the lunar distance at the time.

Laser ranging

[edit]
Lunar Laser Ranging Experiment from the Apollo 11 mission

An experiment which measured the round-trip time of flight of laser pulses reflected directly off the surface of the Moon was performed in 1962, by a team from Massachusetts Institute of Technology, and a Soviet team at the Crimean Astrophysical Observatory.[48]

During the Apollo missions in 1969, astronauts placed retroreflectors on the surface of the Moon for the purpose of refining the accuracy and precision of this technique. The measurements are ongoing and involve multiple laser facilities. The instantaneous precision of the Lunar Laser Ranging experiments can achieve small millimeter resolution, and is the most reliable method of determining the lunar distance. The semi-major axis is determined to be 384,399.0 km.[10]

Amateur astronomers and citizen scientists

[edit]

Due to the modern accessibility of accurate timing devices, high resolution digital cameras, GPS receivers, powerful computers and near-instantaneous communication, it has become possible for amateur astronomers to make high accuracy measurements of the lunar distance.

On May 23, 2007, digital photographs of the Moon during a near-occultation of Regulus were taken from two locations, in Greece and England. By measuring the parallax between the Moon and the chosen background star, the lunar distance was calculated.[49]

A more ambitious project called the "Aristarchus Campaign" was conducted during the lunar eclipse of 15 April 2014.[21] During this event, participants were invited to record a series of five digital photographs from moonrise until culmination (the point of greatest altitude).

The method took advantage of the fact that the Moon is actually closest to an observer when it is at its highest point in the sky, compared to when it is on the horizon. Although it appears that the Moon is biggest when it is near the horizon, the opposite is true. This phenomenon is known as the Moon illusion. The reason for the difference in distance is that the distance from the center of the Moon to the center of the Earth is nearly constant throughout the night, but an observer on the surface of Earth is actually 1 Earth radius from the center of Earth. This offset brings them closest to the Moon when it is overhead.

Modern cameras have achieved a resolution capable of capturing the Moon with enough precision to detect and measure this tiny variation in apparent size. The results of this experiment were calculated as LD = 60.51+3.91
−4.19 R🜨. The accepted value for that night was 60.61 R🜨, which implied a 3% accuracy. The benefit of this method is that the only measuring equipment needed is a modern digital camera (equipped with an accurate clock, and a GPS receiver).

Other experimental methods of measuring the lunar distance that can be performed by amateur astronomers involve:

  • Taking pictures of the Moon before it enters the penumbra and after it is completely eclipsed.
  • Measuring, as precisely as possible, the time of the eclipse contacts.
  • Taking good pictures of the partial eclipse when the shape and size of the Earth shadow are clearly visible.
  • Taking a picture of the Moon including, in the same field of view, Spica and Mars – from various locations.

See also

[edit]

References

[edit]
  1. ^ "NEO Earth Close Approaches". Neo.jpl.nasa.gov. Archived from the original on 2014-03-07. Retrieved 2016-02-22.
  2. ^ Williams, J. G.; Newhall, X. X.; Dickey, J. O. (15 June 1996). "Relativity parameters determined from lunar laser ranging" (PDF). Physical Review D. 53 (12): 6730–6739. Bibcode:1996PhRvD..53.6730W. doi:10.1103/PhysRevD.53.6730. PMID 10019959.
  3. ^ Shuch, H. Paul (July 1991). "Measuring the mass of the earth: the ultimate moonbounce experiment" (PDF). Proceedings, 25th Conference of the Central States VHF Society: 25–30. Retrieved 28 February 2016.
  4. ^ a b Fischer, Irene (August 1962). "Parallax of the moon in terms of a world geodetic system" (PDF). The Astronomical Journal. 67: 373. Bibcode:1962AJ.....67..373F. doi:10.1086/108742.
  5. ^ Dickey, J. O.; Bender, P. L.; et al. (22 July 1994). "Lunar Laser Ranging: A Continuing Legacy of the Apollo Program" (PDF). Science. 265 (5171): 482–490. Bibcode:1994Sci...265..482D. doi:10.1126/science.265.5171.482. PMID 17781305. S2CID 10157934.
  6. ^ "Is the Moon moving away from the Earth? When was this discovered? (Intermediate) - Curious About Astronomy? Ask an Astronomer". Curious.astro.cornell.edu. Retrieved 2016-02-22.
  7. ^ C.D. Murray & S.F. Dermott (1999). Solar System Dynamics. Cambridge University Press. p. 184.
  8. ^ Dickinson, Terence (1993). From the Big Bang to Planet X. Camden East, Ontario: Camden House. pp. 79–81. ISBN 978-0-921820-71-0.
  9. ^ a b Meeus: Mathematical Astronomy Morsels. Willmann-Bell, Richmond 1997, ISBN 0-943396-51-4, Kapitel 4. See German Wikipedia article for more information.
  10. ^ a b Williams, James G.; Dickey, Jean O. (2002). "Lunar geophysics, geodesy and dynamics". In Ron Noomen; Steven Klosko; Carey Noll; Michael Pearlman (eds.). 13th International Workshop on Laser Ranging. Goddard Space Flight Center.
  11. ^ J. L. Simon, P. Bretagnon, J. Chapront, M. Chapront-Touze, G. Francou, J. Laskar (Feb 1994). "Numerical expressions for precession formulae and mean elements for the Moon and the planets". Astronomy and Astrophysics. 282: 663. Bibcode:1994A&A...282..663S.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  12. ^ Meeus: Mathematical Astronomy Morsels. Willmann-Bell, Richmond 1997, ISBN 0-943396-51-4, Kapitel 2.
  13. ^ a b c d Battat, J. B. R.; Murphy, T. W.; Adelberger, E. G. (January 2009). "The Apache Point Observatory Lunar Laser-ranging Operation (APOLLO): Two Years of Millimeter-Precision Measurements of the Earth-Moon Range". Astronomical Society of the Pacific. 121 (875): 29–40. Bibcode:2009PASP..121...29B. doi:10.1086/596748. JSTOR 10.1086/596748.
  14. ^ Lasater, A. Brian (2007). The dream of the West : the ancient heritage and the European achievement in map-making, navigation and science, 1487–1727. Morrisville: Lulu Enterprises. p. 185. ISBN 978-1-4303-1382-3.
  15. ^ Leslie, William T. Fox (1983). At the sea's edge : an introduction to coastal oceanography for the amateur naturalist. Illustrated by Clare Walker. Englewood Cliffs, N.J.: Prentice-Hall. p. 101. ISBN 978-0130497833.
  16. ^ Williams, Dr. David R. (18 November 2015). "Planetary Fact Sheet - Ratio to Earth Values". NASA Goddard Space Flight Center. Retrieved 28 February 2016.
  17. ^ a b Groten, Erwin (1 April 2004). "Fundamental Parameters and Current (2004) Best Estimates of the Parameters of Common Relevance to Astronomy, Geodesy, and Geodynamics by Erwin Groten, IPGD, Darmstadt" (PDF). Journal of Geodesy. 77 (10–11): 724–797. Bibcode:2004JGeod..77..724.. doi:10.1007/s00190-003-0373-y. S2CID 16907886. Retrieved 2 March 2016.
  18. ^ "International Astronomical Union | IAU". www.iau.org. Retrieved 5 May 2019.
  19. ^ Design of a Mars Passenger Ship
  20. ^ Murphy, T W (1 July 2013). "Lunar laser ranging: the millimeter challenge" (PDF). Reports on Progress in Physics. 76 (7): 2. arXiv:1309.6294. Bibcode:2013RPPh...76g6901M. doi:10.1088/0034-4885/76/7/076901. PMID 23764926. S2CID 15744316.
  21. ^ a b Zuluaga, Jorge I.; Figueroa, Juan C.; Ferrin, Ignacio (19 May 2014). "The simplest method to measure the geocentric lunar distance: a case of citizen science". arXiv:1405.4580 [physics.pop-ph].[page needed]
  22. ^ a b Reasenberg, R.D.; Chandler, J.F.; et al. (2016). "Modeling and Analysis of the APOLLO Lunar Laser Ranging Data". arXiv:1608.04758 [astro-ph.IM].
  23. ^ a b Vitagliano, Aldo (1997). "Numerical integration for the real time production of fundamental ephemerides over a wide time span" (PDF). Celestial Mechanics and Dynamical Astronomy. 66 (3): 293–308. Bibcode:1996CeMDA..66..293V. doi:10.1007/BF00049383. S2CID 119510653.
  24. ^ Park, Ryan S.; Folkner, William M.; Williams, James G.; Boggs, Dale H. (2021). "The JPL Planetary and Lunar Ephemerides DE440 and DE441". The Astronomical Journal. 161 (3): 105. Bibcode:2021AJ....161..105P. doi:10.3847/1538-3881/abd414. ISSN 1538-3881.
  25. ^ a b Folkner, W. M.; Williams, J. G.; et al. (February 2014). "The Planetary and Lunar Ephemerides DE430 and DE431" (PDF). The Interplanetary Network Progress Report. 42–169: 1. Bibcode:2014IPNPR.196C...1F.
  26. ^ a b Winter, Niels J.; Goderis, Steven; Van Malderen, Stijn J.M.; et al. (18 February 2020). "Subdaily-Scale Chemical Variability in a Rudist Shell: Implications for Rudist Paleobiology and the Cretaceous Day-Night Cycle". Paleoceanography and Paleoclimatology. 35 (2). doi:10.1029/2019PA003723. hdl:1854/LU-8685501.
  27. ^ Choi, Charles Q. (19 November 2014). "Moon Facts: Fun Information About the Earth's Moon". Space.com. TechMediaNetworks, Inc. Retrieved 3 March 2016.
  28. ^ a b Williams, James G.; Boggs, Dale H. (2016). "Secular tidal changes in lunar orbit and Earth rotation". Celestial Mechanics and Dynamical Astronomy. 126 (1): 89–129. Bibcode:2016CeMDA.126...89W. doi:10.1007/s10569-016-9702-3. ISSN 1572-9478. S2CID 124256137.
  29. ^ Stephenson, F. R.; Morrison, L. V.; Hohenkerk, C. Y. (2016). "Measurement of the Earth's rotation: 720 BC to AD 2015". Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences. 472 (2196): 20160404. Bibcode:2016RSPSA.47260404S. doi:10.1098/rspa.2016.0404. PMC 5247521. PMID 28119545.
  30. ^ Morrison, L. V.; Stephenson, F. R.; Hohenkerk, C. Y.; Zawilski, M. (2021). "Addendum 2020 to 'Measurement of the Earth's rotation: 720 BC to AD 2015". Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences. 477 (2246): 20200776. Bibcode:2021RSPSA.47700776M. doi:10.1098/rspa.2020.0776. S2CID 231938488.
  31. ^ a b Walker, James C. G.; Zahnle, Kevin J. (17 April 1986). "Lunar nodal tide and distance to the Moon during the Precambrian" (PDF). Nature. 320 (6063): 600–602. Bibcode:1986Natur.320..600W. doi:10.1038/320600a0. hdl:2027.42/62576. PMID 11540876. S2CID 4350312.
  32. ^ Bills, B.G. & Ray, R.D. (1999), "Lunar Orbital Evolution: A Synthesis of Recent Results", Geophysical Research Letters, 26 (19): 3045–3048, Bibcode:1999GeoRL..26.3045B, doi:10.1029/1999GL008348
  33. ^ Cain, Fraser (2016-04-12). "WHEN WILL EARTH LOCK TO THE MOON?". Universe Today. Retrieved 1 September 2016.
  34. ^ Canup, R. M. (17 October 2012). "Forming a Moon with an Earth-like Composition via a Giant Impact". Science. 338 (6110): 1052–1055. Bibcode:2012Sci...338.1052C. doi:10.1126/science.1226073. PMC 6476314. PMID 23076098.
  35. ^ "The Theia Hypothesis: New Evidence Emerges that Earth and Moon Were Once the Same". The Daily Galaxy. 2007-07-05. Retrieved 2013-11-13.
  36. ^ Newhall, X.X; Standish, E.M; Williams, J. G. (Aug 1983). "DE 102 - A numerically integrated ephemeris of the moon and planets spanning forty-four centuries". Astronomy and Astrophysics. 125 (1): 150–167. Bibcode:1983A&A...125..150N. ISSN 0004-6361. Retrieved 28 February 2016.
  37. ^ Gutzwiller, Martin C. (1998). "Moon–Earth–Sun: The oldest three-body problem". Reviews of Modern Physics. 70 (2): 589–639. Bibcode:1998RvMP...70..589G. doi:10.1103/RevModPhys.70.589.
  38. ^ Sheehan, William; Westfall, John (2004). The transits of Venus. Amherst, N.Y.: Prometheus Books. pp. 27–28. ISBN 978-1-59102-175-9.
  39. ^ Webb, Stephen (1999), "3.2 Aristarchus, Hipparchus, and Ptolemy", Measuring the Universe: The Cosmological Distance Ladder, Springer, pp. 27–35, ISBN 978-1-85233-106-1. See in particular p. 33: "Almost everything we know about Hipparchus comes down to us by way of Ptolemy."
  40. ^ Helden, Albert van (1986). Measuring the universe : cosmic dimensions from Aristarchus to Halley (Repr. ed.). Chicago: University of Chicago Press. p. 16. ISBN 978-0-226-84882-2.
  41. ^ Fischer, Irène (7 November 2008). "The distance of the moon". Bulletin Géodésique. 71 (1): 37–63. Bibcode:1964BGeod..38...37F. doi:10.1007/BF02526081. S2CID 117060032.
  42. ^ O'Keefe, J. A.; Anderson, J. P. (1952). "The earth's equatorial radius and the distance of the moon" (PDF). Astronomical Journal. 57: 108–121. Bibcode:1952AJ.....57..108O. doi:10.1086/106720.
  43. ^ Gootée, Tom (April 1946). "Radar reaches the moon" (PDF). Radio News. 35 (4). Ziff-Davis Publishing Co.: 25–27. Bibcode:1946RaNew..35...25G. Retrieved September 9, 2014.
  44. ^ "Project Diana hits the Moon… in 1946". SciHi Blog. 2022-01-10. Retrieved 2023-01-29.
  45. ^ Yaplee, B. S.; Roman, N. G.; Scanlan, T. F.; Craig, K. J. (30 July – 6 August 1958). "A lunar radar study at 10-cm wavelength". Paris Symposium on Radio Astronomy. IAU Symposium no. 9 (9): 19. Bibcode:1959IAUS....9...19Y.
  46. ^ Hey, J. S.; Hughes, V. A. (30 July – 6 August 1958). "Radar observation of the moon at 10-cm wavelength". Paris Symposium on Radio Astronomy. 9 (9): 13–18. Bibcode:1959IAUS....9...13H. doi:10.1017/s007418090005049x.
  47. ^ Yaplee, B. S.; Knowles, S. H.; et al. (January 1965). "The mean distance to the Moon as determined by radar". Symposium - International Astronomical Union. 21: 2. Bibcode:1965IAUS...21...81Y. doi:10.1017/S0074180900104826.
  48. ^ Bender, P. L.; Currie, D. G.; Dicke, R. H.; et al. (October 19, 1973). "The Lunar Laser Ranging Experiment" (PDF). Science. 182 (4109): 229–238. Bibcode:1973Sci...182..229B. doi:10.1126/science.182.4109.229. PMID 17749298. S2CID 32027563. Retrieved April 27, 2013.
  49. ^ Wright, Ernie. "Overhead view of the Earth-Moon system, to scale Lunar Parallax: Estimating the Moon's Distance". Retrieved 29 February 2016.
[edit]
Retrieved from "https://en.wikipedia.org/w/index.php?title=Lunar_distance&oldid=1254425243"