In physics and classical mechanics, the **three-body problem** is the problem of taking the initial positions and velocities (or momenta) of three point masses and solving for their subsequent motion according to Newton's laws of motion and Newton's law of universal gravitation.^{ [1] } The three-body problem is a special case of the n-body problem. Unlike two-body problems, no general closed-form solution exists,^{ [1] } as the resulting dynamical system is chaotic for most initial conditions, and numerical methods are generally required.

- Mathematical description
- Restricted three-body problem
- Solutions
- General solution
- Special-case solutions
- Numerical approaches
- History
- Other problems involving three bodies
- n-body problem
- In popular culture
- See also
- References
- Further reading
- External links

Historically, the first specific three-body problem to receive extended study was the one involving the Moon, the Earth, and the Sun.^{ [2] } In an extended modern sense, a three-body problem is any problem in classical mechanics or quantum mechanics that models the motion of three particles.

The mathematical statement of the three-body problem can be given in terms of the Newtonian equations of motion for vector positions of three gravitationally interacting bodies with masses :

where is the gravitational constant.^{ [3] }^{ [4] } This is a set of 9 second-order differential equations. The problem can also be stated equivalently in the Hamiltonian formalism, in which case it is described by a set of 18 first-order differential equations, one for each component of the positions and momenta :

where is the Hamiltonian:

In this case is simply the total energy of the system, gravitational plus kinetic.

In the *restricted three-body problem*,^{ [3] } a body of negligible mass (the "planetoid") moves under the influence of two massive bodies. Having negligible mass, the force that the planetoid exerts on the two massive bodies may be neglected, and the system can be analysed and can therefore be described in terms of a two-body motion. Usually this two-body motion is taken to consist of circular orbits around the center of mass, and the planetoid is assumed to move in the plane defined by the circular orbits.

The restricted three-body problem is easier to analyze theoretically than the full problem. It is of practical interest as well since it accurately describes many real-world problems, the most important example being the Earth–Moon–Sun system. For these reasons, it has occupied an important role in the historical development of the three-body problem.

Mathematically, the problem is stated as follows. Let be the masses of the two massive bodies, with (planar) coordinates and , and let be the coordinates of the planetoid. For simplicity, choose units such that the distance between the two massive bodies, as well as the gravitational constant, are both equal to . Then, the motion of the planetoid is given by

where . In this form the equations of motion carry an explicit time dependence through the coordinates . However, this time-dependence can be removed through a transformation to a rotating reference frame, which simplifies any subsequent analysis.

There is no general analytical solution to the three-body problem given by simple algebraic expressions and integrals.^{ [1] } Moreover, the motion of three bodies is generally non-repeating, except in special cases.^{ [5] }

On the other hand, in 1912 the Finnish mathematician Karl Fritiof Sundman proved that there exists a series solution in powers of *t*^{1/3} for the 3-body problem.^{ [6] } This series converges for all real t, except for initial conditions corresponding to zero angular momentum. (In practice the latter restriction is insignificant since such initial conditions are rare, having Lebesgue measure zero.)

An important issue in proving this result is the fact that the radius of convergence for this series is determined by the distance to the nearest singularity. Therefore, it is necessary to study the possible singularities of the 3-body problems. As it will be briefly discussed below, the only singularities in the 3-body problem are binary collisions (collisions between two particles at an instant) and triple collisions (collisions between three particles at an instant).

Collisions, whether binary or triple (in fact, any number), are somewhat improbable, since it has been shown that they correspond to a set of initial conditions of measure zero. However, there is no criterion known to be put on the initial state in order to avoid collisions for the corresponding solution. So Sundman's strategy consisted of the following steps:

- Using an appropriate change of variables to continue analyzing the solution beyond the binary collision, in a process known as regularization.
- Proving that triple collisions only occur when the angular momentum
**L**vanishes. By restricting the initial data to**L**≠**0**, he removed all*real*singularities from the transformed equations for the 3-body problem. - Showing that if
**L**≠**0**, then not only can there be no triple collision, but the system is strictly bounded away from a triple collision. This implies, by using Cauchy's existence theorem for differential equations, that there are no complex singularities in a strip (depending on the value of**L**) in the complex plane centered around the real axis (shades of Kovalevskaya). - Find a conformal transformation that maps this strip into the unit disc. For example, if
*s*=*t*^{1/3}(the new variable after the regularization) and if |ln*s*| ≤*β*,^{[ clarification needed ]}then this map is given by

This finishes the proof of Sundman's theorem.

Unfortunately, the corresponding series converges very slowly. That is, obtaining a value of meaningful precision requires so many terms that this solution is of little practical use. Indeed, in 1930, David Beloriszky calculated that if Sundman's series were to be used for astronomical observations, then the computations would involve at least 10^{8000000} terms.^{ [7] }

In 1767, Leonhard Euler found three families of periodic solutions in which the three masses are collinear at each instant. See Euler's three-body problem.

In 1772, Lagrange found a family of solutions in which the three masses form an equilateral triangle at each instant. Together with Euler's collinear solutions, these solutions form the central configurations for the three-body problem. These solutions are valid for any mass ratios, and the masses move on Keplerian ellipses. These four families are the only known solutions for which there are explicit analytic formulae. In the special case of the circular restricted three-body problem, these solutions, viewed in a frame rotating with the primaries, become points which are referred to as L_{1}, L_{2}, L_{3}, L_{4}, and L_{5}, and called Lagrangian points, with L_{4} and L_{5} being symmetric instances of Lagrange's solution.

In work summarized in 1892–1899, Henri Poincaré established the existence of an infinite number of periodic solutions to the restricted three-body problem, together with techniques for continuing these solutions into the general three-body problem.

In 1893, Meissel stated what is now called the Pythagorean three-body problem: three masses in the ratio 3:4:5 are placed at rest at the vertices of a 3:4:5 right triangle. Burrau^{ [8] } further investigated this problem in 1913. In 1967 Victor Szebehely and C. Frederick Peters established eventual escape for this problem using numerical integration, while at the same time finding a nearby periodic solution.^{ [9] }

In the 1970s, Michel Hénon and Roger A. Broucke each found a set of solutions that form part of the same family of solutions: the Broucke–Henon–Hadjidemetriou family. In this family the three objects all have the same mass and can exhibit both retrograde and direct forms. In some of Broucke's solutions two of the bodies follow the same path.^{ [10] }

In 1993, a zero angular momentum solution with three equal masses moving around a figure-eight shape was discovered numerically by physicist Cris Moore at the Santa Fe Institute.^{ [12] } Its formal existence was later proved in 2000 by mathematicians Alain Chenciner and Richard Montgomery.^{ [13] }^{ [14] } The solution has been shown numerically to be stable for small perturbations of the mass and orbital parameters, which raises the intriguing possibility that such orbits could be observed in the physical universe. However, it has been argued that this occurrence is unlikely since the domain of stability is small. For instance, the probability of a binary–binary scattering event^{[ clarification needed ]} resulting in a figure-8 orbit has been estimated to be a small fraction of 1%.^{ [15] }

In 2013, physicists Milovan Šuvakov and Veljko Dmitrašinović at the Institute of Physics in Belgrade discovered 13 new families of solutions for the equal-mass zero-angular-momentum three-body problem.^{ [5] }^{ [10] }

In 2015, physicist Ana Hudomal discovered 14 new families of solutions for the equal-mass zero-angular-momentum three-body problem.^{ [16] }

In 2017, researchers Xiaoming Li and Shijun Liao found 669 new periodic orbits of the equal-mass zero-angular-momentum three-body problem.^{ [17] } This was followed in 2018 by an additional 1223 new solutions for a zero-momentum system of unequal masses.^{ [18] }

In 2018, Li and Liao reported 234 solutions to the unequal-mass "free-fall" three body problem.^{ [19] } The free fall formulation of the three body problem starts with all three bodies at rest. Because of this, the masses in a free-fall configuration do not orbit in a closed "loop", but travel forwards and backwards along an open "track".

Using a computer, the problem may be solved to arbitrarily high precision using numerical integration although high precision requires a large amount of CPU time. In 2019, Breen et al. announced a fast neural network solver, trained using a numerical integrator.^{ [20] }

The gravitational problem of three bodies in its traditional sense dates in substance from 1687, when Isaac Newton published his *Principia* (* Philosophiæ Naturalis Principia Mathematica *). In Proposition 66 of Book 1 of the *Principia*, and its 22 Corollaries, Newton took the first steps in the definition and study of the problem of the movements of three massive bodies subject to their mutually perturbing gravitational attractions. In Propositions 25 to 35 of Book 3, Newton also took the first steps in applying his results of Proposition 66 to the lunar theory, the motion of the Moon under the gravitational influence of the Earth and the Sun.

The physical problem was addressed by Amerigo Vespucci and subsequently by Galileo Galilei; in 1499, Vespucci used knowledge of the position of the Moon to determine his position in Brazil. It became of technical importance in the 1720s, as an accurate solution would be applicable to navigation, specifically for the determination of longitude at sea, solved in practice by John Harrison's invention of the marine chronometer. However the accuracy of the lunar theory was low, due to the perturbing effect of the Sun and planets on the motion of the Moon around the Earth.

Jean le Rond d'Alembert and Alexis Clairaut, who developed a longstanding rivalry, both attempted to analyze the problem in some degree of generality; they submitted their competing first analyses to the Académie Royale des Sciences in 1747.^{ [21] } It was in connection with their research, in Paris during the 1740s, that the name "three-body problem" (French : *Problème des trois Corps*) began to be commonly used. An account published in 1761 by Jean le Rond d'Alembert indicates that the name was first used in 1747.^{ [22] }

The term 'three-body problem' is sometimes used in the more general sense to refer to any physical problem involving the interaction of three bodies.

A quantum mechanical analogue of the gravitational three-body problem in classical mechanics is the helium atom, in which a helium nucleus and two electrons interact according to the inverse-square Coulomb interaction. Like the gravitational three-body problem, the helium atom cannot be solved exactly.^{ [23] }

In both classical and quantum mechanics, however, there exist nontrivial interaction laws besides the inverse-square force which do lead to exact analytic three-body solutions. One such model consists of a combination of harmonic attraction and a repulsive inverse-cube force.^{ [24] } This model is considered nontrivial since it is associated with a set of nonlinear differential equations containing singularities (compared with, e.g., harmonic interactions alone, which lead to an easily solved system of linear differential equations). In these two respects it is analogous to (insoluble) models having Coulomb interactions, and as a result has been suggested as a tool for intuitively understanding physical systems like the helium atom.^{ [24] }^{ [25] }

The gravitational three-body problem has also been studied using general relativity. Physically, a relativistic treatment becomes necessary in systems with very strong gravitational fields, such as near the event horizon of a black hole. However, the relativistic problem is considerably more difficult than in Newtonian mechanics, and sophisticated numerical techniques are required. Even the full two-body problem (i.e. for arbitrary ratio of masses) does not have a rigorous analytic solution in general relativity.^{ [26] }

The three-body problem is a special case of the n-body problem, which describes how n objects will move under one of the physical forces, such as gravity. These problems have a global analytical solution in the form of a convergent power series, as was proven by Karl F. Sundman for *n* = 3 and by Qiudong Wang for *n* > 3 (see n-body problem for details). However, the Sundman and Wang series converge so slowly that they are useless for practical purposes;^{ [27] } therefore, it is currently necessary to approximate solutions by numerical analysis in the form of numerical integration or, for some cases, classical trigonometric series approximations (see n-body simulation). Atomic systems, e.g. atoms, ions, and molecules, can be treated in terms of the quantum n-body problem. Among classical physical systems, the n-body problem usually refers to a galaxy or to a cluster of galaxies; planetary systems, such as stars, planets, and their satellites, can also be treated as n-body systems. Some applications are conveniently treated by perturbation theory, in which the system is considered as a two-body problem plus additional forces causing deviations from a hypothetical unperturbed two-body trajectory.

- The problem is a plot device in the science fiction trilogy by Chinese author Cixin Liu, and its name has been used for both the first volume and the trilogy as a whole.
^{ [28] }

In physics, **angular momentum** is the rotational equivalent of linear momentum. It is an important quantity in physics because it is a conserved quantity—the total angular momentum of a closed system remains constant.

In physics, an **orbit** is the gravitationally curved trajectory of an object, such as the trajectory of a planet around a star or a natural satellite around a planet. Normally, orbit refers to a regularly repeating trajectory, although it may also refer to a non-repeating trajectory. To a close approximation, planets and satellites follow elliptic orbits, with the center of mass being orbited at a focal point of the ellipse, as described by Kepler's laws of planetary motion.

The **Schrödinger equation** is a linear partial differential equation that describes the wave function or state function of a quantum-mechanical system. It is a key result in quantum mechanics, and its discovery was a significant landmark in the development of the subject. The equation is named after Erwin Schrödinger, who postulated the equation in 1925, and published it in 1926, forming the basis for the work that resulted in his Nobel Prize in Physics in 1933.

In physics, the **reduced mass** is the "effective" inertial mass appearing in the two-body problem of Newtonian mechanics. It is a quantity which allows the two-body problem to be solved as if it were a one-body problem. Note, however, that the mass determining the gravitational force is *not* reduced. In the computation one mass *can* be replaced with the reduced mass, if this is compensated by replacing the other mass with the sum of both masses. The reduced mass is frequently denoted by (mu), although the standard gravitational parameter is also denoted by . It has the dimensions of mass, and SI unit kg.

In physics, the **center of mass** of a distribution of mass in space is the unique point where the weighted relative position of the distributed mass sums to zero. This is the point to which a force may be applied to cause a linear acceleration without an angular acceleration. Calculations in mechanics are often simplified when formulated with respect to the center of mass. It is a hypothetical point where the entire mass of an object may be assumed to be concentrated to visualise its motion. In other words, the center of mass is the particle equivalent of a given object for application of Newton's laws of motion.

**Newton's law of universal gravitation** is usually stated as that every particle attracts every other particle in the universe with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between their centers. The publication of the theory has become known as the "first great unification", as it marked the unification of the previously described phenomena of gravity on Earth with known astronomical behaviors.

In classical mechanics, the **two-body problem** is to predict the motion of two massive objects which are abstractly viewed as point particles. The problem assumes that the two objects interact only with one another; the only force affecting each object arises from the other one, and all other objects are ignored.

**Stellar dynamics** is the branch of astrophysics which describes in a statistical way the collective motions of stars subject to their mutual gravity. The essential difference from celestial mechanics is that each star contributes more or less equally to the total gravitational field, whereas in celestial mechanics the pull of a massive body dominates any satellite orbits.

In classical mechanics, the **gravitational potential** at a location is equal to the work per unit mass that would be needed to move an object to that location from a fixed reference location. It is analogous to the electric potential with mass playing the role of charge. The reference location, where the potential is zero, is by convention infinitely far away from any mass, resulting in a negative potential at any finite distance.

In classical mechanics, the **Laplace–Runge–Lenz (LRL) vector** is a vector used chiefly to describe the shape and orientation of the orbit of one astronomical body around another, such as a planet revolving around a star. For two bodies interacting by Newtonian gravity, the LRL vector is a constant of motion, meaning that it is the same no matter where it is calculated on the orbit; equivalently, the LRL vector is said to be *conserved*. More generally, the LRL vector is conserved in all problems in which two bodies interact by a central force that varies as the inverse square of the distance between them; such problems are called Kepler problems.

In astrodynamics or celestial mechanics, an **elliptic orbit** or **elliptical orbit** is a Kepler orbit with an eccentricity of less than 1; this includes the special case of a circular orbit, with eccentricity equal to 0. In a stricter sense, it is a Kepler orbit with the eccentricity greater than 0 and less than 1. In a wider sense, it is a Kepler's orbit with negative energy. This includes the radial elliptic orbit, with eccentricity equal to 1.

A **classical field theory** is a physical theory that predicts how one or more physical fields interact with matter through **field equations**. The term 'classical field theory' is commonly reserved for describing those physical theories that describe electromagnetism and gravitation, two of the fundamental forces of nature. Theories that incorporate quantum mechanics are called quantum field theories.

In astronomy, **perturbation** is the complex motion of a massive body subject to forces other than the gravitational attraction of a single other massive body. The other forces can include a third body, resistance, as from an atmosphere, and the off-center attraction of an oblate or otherwise misshapen body.

In physics and astronomy, **Euler's three-body problem** is to solve for the motion of a particle that is acted upon by the gravitational field of two other point masses that are fixed in space. This problem is exactly solvable, and yields an approximate solution for particles moving in the gravitational fields of prolate and oblate spheroids. This problem is named after Leonhard Euler, who discussed it in memoirs published in 1760. Important extensions and analyses were contributed subsequently by Lagrange, Liouville, Laplace, Jacobi, Darboux, Le Verrier, Velde, Hamilton, Poincaré, Birkhoff and E. T. Whittaker, among others.

The **Schrödinger–Newton equation**, sometimes referred to as the **Newton–Schrödinger** or **Schrödinger–Poisson equation**, is a nonlinear modification of the Schrödinger equation with a Newtonian gravitational potential, where the gravitational potential emerges from the treatment of the wave function as a mass density, including a term that represents interaction of a particle with its own gravitational field. The inclusion of a self-interaction term represents a fundamental alteration of quantum mechanics. It can be written either as a single integro-differential equation or as a coupled system of a Schrödinger and a Poisson equation. In the latter case it is also referred to in the plural form.

In classical mechanics, the **Kepler problem** is a special case of the two-body problem, in which the two bodies interact by a central force *F* that varies in strength as the inverse square of the distance *r* between them. The force may be either attractive or repulsive. The problem is to find the position or speed of the two bodies over time given their masses, positions, and velocities. Using classical mechanics, the solution can be expressed as a Kepler orbit using six orbital elements.

The **two-body problem in general relativity** is the determination of the motion and gravitational field of two bodies as described by the field equations of general relativity. Solving the Kepler problem is essential to calculate the bending of light by gravity and the motion of a planet orbiting its sun. Solutions are also used to describe the motion of binary stars around each other, and estimate their gradual loss of energy through gravitational radiation.

In celestial mechanics, a **Kepler orbit** is the motion of one body relative to another, as an ellipse, parabola, or hyperbola, which forms a two-dimensional orbital plane in three-dimensional space. A Kepler orbit can also form a straight line. It considers only the point-like gravitational attraction of two bodies, neglecting perturbations due to gravitational interactions with other objects, atmospheric drag, solar radiation pressure, a non-spherical central body, and so on. It is thus said to be a solution of a special case of the two-body problem, known as the Kepler problem. As a theory in classical mechanics, it also does not take into account the effects of general relativity. Keplerian orbits can be parametrized into six orbital elements in various ways.

In physics, the **n-body problem** is the problem of predicting the individual motions of a group of celestial objects interacting with each other gravitationally. Solving this problem has been motivated by the desire to understand the motions of the Sun, Moon, planets, and visible stars. In the 20th century, understanding the dynamics of globular cluster star systems became an important n-body problem. The n-body problem in general relativity is considerably more difficult to solve.

**Orbit modeling** is the process of creating mathematical models to simulate motion of a massive body as it moves in orbit around another massive body due to gravity. Other forces such as gravitational attraction from tertiary bodies, air resistance, solar pressure, or thrust from a propulsion system are typically modeled as secondary effects. Directly modeling an orbit can push the limits of machine precision due to the need to model small perturbations to very large orbits. Because of this, perturbation methods are often used to model the orbit in order to achieve better accuracy.

- 1 2 3 Barrow-Green, June (2008), "The Three-Body Problem", in Gowers, Timothy; Barrow-Green, June; Leader, Imre (eds.),
*The Princeton Companion to Mathematics*, Princeton University Press, pp. 726–728 - ↑ "Historical Notes: Three-Body Problem" . Retrieved 19 July 2017.
- 1 2 Barrow-Green, June (1997).
*Poincaré and the Three Body Problem*. American Mathematical Soc. pp. 8–12. Bibcode:1997ptbp.book.....B. ISBN 978-0-8218-0367-7. - ↑ The Three-Body Problem
- 1 2 Cartwright, Jon (8 March 2013). "Physicists Discover a Whopping 13 New Solutions to Three-Body Problem".
*Science Now*. Retrieved 2013-04-04. - ↑ Barrow-Green, J. (2010). The dramatic episode of Sundman, Historia Mathematica 37, pp. 164–203.
- ↑ Beloriszky, D. (1930). "Application pratique des méthodes de M. Sundman à un cas particulier du problème des trois corps".
*Bulletin Astronomique*. Série 2.**6**: 417–434. Bibcode:1930BuAst...6..417B. - ↑ Burrau (1913). "Numerische Berechnung eines Spezialfalles des Dreikörperproblems".
*Astronomische Nachrichten*.**195**(6): 113–118. Bibcode:1913AN....195..113B. doi:10.1002/asna.19131950602. - ↑ Victor Szebehely; C. Frederick Peters (1967). "Complete Solution of a General Problem of Three Bodies".
*Astronomical Journal*.**72**: 876. Bibcode:1967AJ.....72..876S. doi:10.1086/110355. - 1 2 Šuvakov, M.; Dmitrašinović, V. "Three-body Gallery" . Retrieved 12 August 2015.
- ↑ Here the gravitational constant
*G*has been set to 1, and the initial conditions are**r**_{1}(0) = −**r**_{3}(0) = (−0.97000436, 0.24308753);**r**_{2}(0) = (0,0);**v**_{1}(0) =**v**_{3}(0) = (0.4662036850, 0.4323657300);**v**_{2}(0) = (−0.93240737, −0.86473146). The values are obtained from Chenciner & Montgomery (2000). - ↑ Moore, Cristopher (1993), "Braids in classical dynamics" (PDF),
*Physical Review Letters*,**70**(24): 3675–3679, Bibcode:1993PhRvL..70.3675M, doi:10.1103/PhysRevLett.70.3675, PMID 10053934 - ↑ Chenciner, Alain; Montgomery, Richard (2000). "A remarkable periodic solution of the three-body problem in the case of equal masses".
*Annals of Mathematics*. Second Series.**152**(3): 881–902. arXiv: math/0011268 . Bibcode:2000math.....11268C. doi:10.2307/2661357. JSTOR 2661357. - ↑ Montgomery, Richard (2001), "A new solution to the three-body problem" (PDF),
*Notices of the American Mathematical Society*,**48**: 471–481 - ↑ Heggie, Douglas C. (2000), "A new outcome of binary–binary scattering",
*Monthly Notices of the Royal Astronomical Society*,**318**(4): L61–L63, arXiv: astro-ph/9604016 , Bibcode:2000MNRAS.318L..61H, doi:10.1046/j.1365-8711.2000.04027.x - ↑ Hudomal, Ana (October 2015). "New periodic solutions to the three-body problem and gravitational waves" (PDF).
*Master of Science Thesis at the Faculty of Physics, Belgrade University*. Retrieved 5 February 2019. - ↑ Li, Xiaoming; Liao, Shijun (December 2017). "More than six hundreds new families of Newtonian periodic planar collisionless three-body orbits".
*Science China Physics, Mechanics & Astronomy*.**60**(12): 129511. arXiv: 1705.00527 . Bibcode:2017SCPMA..60l9511L. doi:10.1007/s11433-017-9078-5. ISSN 1674-7348. - ↑ Li, Xiaoming; Jing, Yipeng; Liao, Shijun (13 September 2017). "The 1223 new periodic orbits of planar three-body problem with unequal mass and zero angular momentum". arXiv: 1709.04775 . doi:10.1093/pasj/psy057.Cite journal requires
`|journal=`

(help) - ↑ Li, Xiaoming; Liao, Shijun (2019). "Collisionless periodic orbits in the free-fall three-body problem".
*New Astronomy*.**70**: 22–26. arXiv: 1805.07980 . Bibcode:2019NewA...70...22L. doi:10.1016/j.newast.2019.01.003. - ↑ Breen, Philip G.; Foley, Christopher N.; Boekholt, Tjarda; Portegies Zwart, Simon (2019). "Newton vs the machine: Solving the chaotic three-body problem using deep neural networks". arXiv: 1910.07291 . doi:10.1093/mnras/staa713.Cite journal requires
`|journal=`

(help) - ↑ The 1747 memoirs of both parties can be read in the volume of
*Histoires*(including*Mémoires*) of the Académie Royale des Sciences for 1745 (belatedly published in Paris in 1749) (in French):- Clairaut: "On the System of the World, according to the principles of Universal Gravitation" (at pp. 329–364); and
- d'Alembert: "General method for determining the orbits and the movements of all the planets, taking into account their mutual actions" (at pp. 365–390).

- ↑ Jean le Rond d'Alembert, in a paper of 1761 reviewing the mathematical history of the problem, mentions that Euler had given a method for integrating a certain differential equation "in 1740 (seven years before there was question of the Problem of Three Bodies)": see d'Alembert, "Opuscules Mathématiques", vol. 2, Paris 1761, Quatorzième Mémoire ("Réflexions sur le Problème des trois Corps, avec de Nouvelles Tables de la Lune ...") pp. 329–312, at sec. VI, p. 245.
- ↑ Griffiths, David J. (2004).
*Introduction to Quantum Mechanics (2nd ed.)*. Prentice Hall. p. 311. ISBN 978-0-13-111892-8. OCLC 40251748. - 1 2 Crandall, R.; Whitnell, R.; Bettega, R. (1984). "Exactly soluble two‐electron atomic model".
*American Journal of Physics*.**52**(5): 438–442. Bibcode:1984AmJPh..52..438C. doi:10.1119/1.13650. - ↑ Calogero, F. (1969). "Solution of a Three‐Body Problem in One Dimension".
*Journal of Mathematical Physics*.**10**(12): 2191–2196. Bibcode:1969JMP....10.2191C. doi:10.1063/1.1664820. - ↑ Musielak, Z E; Quarles, B (2014). "The three-body problem".
*Reports on Progress in Physics*.**77**(6): 065901. arXiv: 1508.02312 . Bibcode:2014RPPh...77f5901M. doi:10.1088/0034-4885/77/6/065901. ISSN 0034-4885. PMID 24913140.CS1 maint: ref=harv (link) - ↑ Florin Diacu. "The Solution of the
*n*-body Problem",*The Mathematical Intelligencer*, 1996. - ↑ Qin, Amy (November 10, 2014). "In a Topsy-Turvy World, China Warms to Sci-Fi".
*The New York Times*. Archived from the original on December 9, 2019. Retrieved February 5, 2020.

- Poincaré, H. (1967).
*New Methods of Celestial Mechanics, 3 vols. (English trans.)*. American Institute of Physics. ISBN 978-1-56396-117-5. - Aarseth, S. J. (2003).
*Gravitational n-Body Simulations*. New York: Cambridge University Press. ISBN 978-0-521-43272-6. - Bagla, J. S. (2005). "Cosmological N-body simulation: Techniques, scope and status".
*Current Science*.**88**: 1088–1100. arXiv: astro-ph/0411043 . Bibcode:2005CSci...88.1088B. - Chambers, J. E.; Wetherill, G. W. (1998). "Making the Terrestrial Planets: N-Body Integrations of Planetary Embryos in Three Dimensions".
*Icarus*.**136**(2): 304–327. Bibcode:1998Icar..136..304C. CiteSeerX 10.1.1.64.7797 . doi:10.1006/icar.1998.6007. - Efstathiou, G.; Davis, M.; White, S. D. M.; Frenk, C. S. (1985). "Numerical techniques for large cosmological N-body simulations".
*Astrophysical Journal*.**57**: 241–260. Bibcode:1985ApJS...57..241E. doi:10.1086/191003. - Hulkower, Neal D. (1978). "The Zero Energy Three Body Problem".
*Indiana University Mathematics Journal*.**27**(3): 409–447. Bibcode:1978IUMJ...27..409H. doi: 10.1512/iumj.1978.27.27030 . - Hulkower, Neal D. (1980). "Central Configurations and Hyperbolic-Elliptic Motion in the Three-Body Problem".
*Celestial Mechanics*.**21**(1): 37–41. Bibcode:1980CeMec..21...37H. doi:10.1007/BF01230244. - Moore, Cristopher (1993), "Braids in classical dynamics" (PDF),
*Physical Review Letters*,**70**(24): 3675–3679, Bibcode:1993PhRvL..70.3675M, doi:10.1103/PhysRevLett.70.3675, PMID 10053934 . - Šuvakov, Milovan; Dmitrašinović, V. (2013). "Three Classes of Newtonian Three-Body Planar Periodic Orbits".
*Physical Review Letters*.**110**(10): 114301. arXiv: 1303.0181 . Bibcode:2013PhRvL.110k4301S. doi:10.1103/PhysRevLett.110.114301. PMID 25166541. - Li, Xiaoming; Liao, Shijun (2014). "On the stability of the three classes of Newtonian three-body planar periodic orbits".
*Science China Physics, Mechanics & Astronomy*.**57**(11): 2121–2126. arXiv: 1312.6796 . Bibcode:2014SCPMA..57.2121L. doi:10.1007/s11433-014-5563-5.

- Chenciner, Alain (2007). "Three body problem".
*Scholarpedia*.**2**(10): 2111. Bibcode:2007SchpJ...2.2111C. doi: 10.4249/scholarpedia.2111 .

This page is based on this Wikipedia article

Text is available under the CC BY-SA 4.0 license; additional terms may apply.

Images, videos and audio are available under their respective licenses.

Text is available under the CC BY-SA 4.0 license; additional terms may apply.

Images, videos and audio are available under their respective licenses.