Celestial mechanics
Classical mechanics 

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Celestial mechanics is the branch of astronomy that deals with the motions of celestial objects. Historically, celestial mechanics applies principles of physics (classical mechanics) to astronomical objects, such as stars and planets, to produce ephemeris data. As an astronomical field of study, celestial mechanics includes the subfields of Orbital mechanics (astrodynamics), which deals with the orbit of an artificial satellite; and Lunar theory, which deals with the orbit of the Moon.
Contents

History of celestial mechanics 1
 Johannes Kepler 1.1
 Isaac Newton 1.2
 JosephLouis Lagrange 1.3
 Simon Newcomb 1.4
 Albert Einstein 1.5
 Examples of problems 2
 Perturbation theory 3
 See also 4
 Notes 5
 References 6
 Further reading 7
 External links 8
History of celestial mechanics
Modern analytic celestial mechanics started over 300 years ago with Isaac Newton's Principia of 1687. The name "celestial mechanics" is more recent than that. Newton wrote that the field should be called "rational mechanics." The term "dynamics" came in a little later with Gottfried Leibniz, and over a century after Newton, PierreSimon Laplace introduced the term "celestial mechanics." Prior to Kepler there was little connection between exact, quantitative prediction of planetary positions, using geometrical or arithmetical techniques, and contemporary discussions of the physical causes of the planets' motion.
Johannes Kepler
Johannes Kepler (1571–1630) was the first to closely integrate the predictive geometrical astronomy, which had been dominant from Ptolemy in the 2nd century to Copernicus, with physical concepts to produce a New Astronomy, Based upon Causes, or Celestial Physics in 1609. His work led to the modern laws of planetary orbits, which he developed using his physical principles and the planetary observations made by Tycho Brahe. Kepler's model greatly improved the accuracy of predictions of planetary motion, years before Isaac Newton developed his law of gravitation in 1686.
Isaac Newton
Isaac Newton (25 December 1642–31 March 1727) is credited with introducing the idea that the motion of objects in the heavens, such as planets, the Sun, and the Moon, and the motion of objects on the ground, like cannon balls and falling apples, could be described by the same set of physical laws. In this sense he unified celestial and terrestrial dynamics. Using Newton's law of universal gravitation, proving Kepler's Laws for the case of a circular orbit is simple. Elliptical orbits involve more complex calculations, which Newton included in his Principia.
JosephLouis Lagrange
After Newton, Lagrange (25 January 1736–10 April 1813) attempted to solve the threebody problem, analyzed the stability of planetary orbits, and discovered the existence of the Lagrangian points. Lagrange also reformulated the principles of classical mechanics, emphasizing energy more than force and developing a method to use a single polar coordinate equation to describe any orbit, even those that are parabolic and hyperbolic. This is useful for calculating the behaviour of planets and comets and such. More recently, it has also become useful to calculate spacecraft trajectories.
Simon Newcomb
Paris, France in May 1886, the international consensus was that all ephemerides should be based on Newcomb's calculations. A further conference as late as 1950 confirmed Newcomb's constants as the international standard.
Albert Einstein
Albert Einstein (14 March 1879–18 April 1955) explained the anomalous precession of Mercury's perihelion in his 1916 paper The Foundation of the General Theory of Relativity. This led astronomers to recognize that Newtonian mechanics did not provide the highest accuracy. Binary pulsars have been observed, the first in 1974, whose orbits not only require the use of General Relativity for their explanation, but whose evolution proves the existence of gravitational radiation, a discovery that led to the 1993 Nobel Physics Prize.
Examples of problems
Celestial motion without additional forces such as thrust of a rocket, is governed by gravitational acceleration of masses due to other masses. A simplification is the nbody problem, where the problem assumes some number n of spherically symmetric masses. In that case, the integration of the accelerations can be well approximated by relatively simple summations.

Examples:
 4body problem: spaceflight to Mars (for parts of the flight the influence of one or two bodies is very small, so that there we have a 2 or 3body problem; see also the patched conic approximation)

3body problem:
 Quasisatellite
 Spaceflight to, and stay at a Lagrangian point
In the case that n=2 (twobody problem), the situation is much simpler than for larger n. Various explicit formulas apply, where in the more general case typically only numerical solutions are possible. It is a useful simplification that is often approximately valid.

Examples:
 A binary star, e.g., Alpha Centauri (approx. the same mass)
 A binary asteroid, e.g., 90 Antiope (approx. the same mass)
A further simplification is based on the "standard assumptions in astrodynamics", which include that one body, the orbiting body, is much smaller than the other, the central body. This is also often approximately valid.

Examples:
 Solar system orbiting the center of the Milky Way
 A planet orbiting the Sun
 A moon orbiting a planet
 A spacecraft orbiting Earth, a moon, or a planet (in the latter cases the approximation only applies after arrival at that orbit)
Either instead of, or on top of the previous simplification, we may assume circular orbits, making distance and orbital speeds, and potential and kinetic energies constant in time. This assumption sacrifices accuracy for simplicity, especially for high eccentricity orbits which are by definition noncircular.

Examples:
 The orbit of the dwarf planet Pluto, ecc. = 0.2488
 The orbit of Mercury, ecc. = 0.2056
 Hohmann transfer orbit
 Gemini 11 flight
 Suborbital flights
Perturbation theory
Perturbation theory comprises mathematical methods that are used to find an approximate solution to a problem which cannot be solved exactly. (It is closely related to methods used in numerical analysis, which are ancient.) The earliest use of perturbation theory was to deal with the otherwise unsolveable mathematical problems of celestial mechanics: Newton's solution for the orbit of the Moon, which moves noticeably differently from a simple Keplerian ellipse because of the competing gravitation of the Earth and the Sun.
Perturbation methods start with a simplified form of the original problem, which is carefully chosen to be exactly solvable. In celestial mechanics, this is usually a Keplerian ellipse, which is correct when there are only two gravitating bodies (say, the Earth and the Moon), or a circular orbit, which is only correct in special cases of twobody motion, but is often close enough for practical use. The solved, but simplified problem is then "perturbed" to make its starting conditions closer to the real problem, such as including the gravitational attraction of a third body (the Sun). The slight changes that result, which themselves may have been simplified yet again, are used as corrections. Because of simplifications introduced along every step of the way, the corrections are never perfect, but even one cycle of corrections often provides a remarkably better approximate solution to the real problem.
There is no requirement to stop at only one cycle of corrections. A partially corrected solution can be reused as the new starting point for yet another cycle of perturbations and corrections. The common difficulty with the method is that usually the corrections progressively make the new solutions very much more complicated, so each cycle is much more difficult to manage than the previous cycle of corrections. Newton is reported to have said, regarding the problem of the Moon's orbit "It causeth my head to ache."^{[1]}
This general procedure – starting with a simplified problem and gradually adding corrections that make the starting point of the corrected problem closer to the real situation – is a widely used mathematical tool in advanced sciences and engineering. It is the natural extension of the "guess, check, and fix" method used anciently with numbers.
See also
 Astrometry is a part of astronomy that deals with measuring the positions of stars and other celestial bodies, their distances and movements.
 Astrodynamics is the study and creation of orbits, especially those of artificial satellites.
 Celestial navigation is a position fixing technique that was the first system devised to help sailors locate themselves on a featureless ocean.
 Dynamics of the celestial spheres concerns preNewtonian explanations of the causes of the motions of the stars and planets.
 Gravitation
 Numerical analysis is a branch of mathematics, pioneered by celestial mechanicians, for calculating approximate numerical answers (such as the position of a planet in the sky) which are too difficult to solve down to a general, exact formula.
 Creating a numerical model of the solar system was the original goal of celestial mechanics, and has only been imperfectly achieved. It continues to motivate research.
 An orbit is the path that an object makes, around another object, whilst under the influence of a source of centripetal force, such as gravity.
 Orbital elements are the parameters needed to specify a Newtonian twobody orbit uniquely.
 Osculating orbit is the temporary Keplerian orbit about a central body that an object would continue on, if other perturbations were not present.
 Retrograde motion
 Satellite is an object that orbits another object (known as its primary). The term is often used to describe an artificial satellite (as opposed to natural satellites, or moons). The common noun moon (not capitalized) is used to mean any natural satellite of the other planets.
 Tidal force
 The Jet Propulsion Laboratory Developmental Ephemeris (JPL DE) is a widely used model of the solar system, which combines celestial mechanics with numerical analysis and astronomical and spacecraft data.
 Two solutions, called VSOP82 and VSOP87 are versions one mathematical theory for the orbits and positions of the major planets, which seeks to provide accurate positions over an extended period of time.
 Lunar theory attempts to account for the motions of the Moon.
Notes
 ^ Cropper, William H. (2004), Great Physicists: The Life and Times of Leading Physicists from Galileo to Hawking, .
References
 Asger Aaboe, Episodes from the Early History of Astronomy, 2001, SpringerVerlag, ISBN 0387951369
 Forest R. Moulton, Introduction to Celestial Mechanics, 1984, Dover, ISBN 0486646874
 John E.Prussing, Bruce A.Conway, Orbital Mechanics, 1993, Oxford Univ.Press
 William M. Smart, Celestial Mechanics, 1961, John Wiley.
 J. M. A. Danby, Fundamentals of Celestial Mechanics, 1992, WillmannBell
 Alessandra Celletti, Ettore Perozzi, Celestial Mechanics: The Waltz of the Planets, 2007, SpringerPraxis, ISBN 038730777X.
 Michael Efroimsky. 2005. Gauge Freedom in Orbital Mechanics. Annals of the New York Academy of Sciences, Vol. 1065, pp. 346374
 Alessandra Celletti, Stability and Chaos in Celestial Mechanics. SpringerPraxis 2010, XVI, 264 p., Hardcover ISBN 9783540851455
Further reading
 Encyclopedia:Celestial mechanics Scholarpedia Expert articles
External links
 Calvert, James B. (20030328), Celestial Mechanics, University of Denver, retrieved 20060821
 Astronomy of the Earth's Motion in Space, highschool level educational web site by David P. Stern
 Newtonian Dynamics Undergraduate level course by Richard Fitzpatrick. This includes Langrangian and Hamiltonian Dynamics and applications to celestial mechanics, gravitational potential theory, the 3body problem and Lunar motion (an example of the 3body problem with the Sun, Moon, and the Earth).
Research
 Marshall Hampton's research page: Central configurations in the nbody problem
Artwork
 Celestial Mechanics is a Planetarium Artwork created by D. S. Hessels and G. Dunne
Course notes
 Professor Tatum's course notes at the University of Victoria
Associations
 Italian Celestial Mechanics and Astrodynamics Association
Simulations
