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, 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 nine 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 closed-form solution to the three-body problem,^{ [1] } meaning there is no general solution that can be expressed in terms of a finite number of standard mathematical operations. Moreover, the motion of three bodies is generally non-repeating, except in special cases.^{ [5] }

However, in 1912 the Finnish mathematician Karl Fritiof Sundman proved that there exists an analytic solution to the three-body problem in the form of a power series in terms of powers of *t*^{1/3}.^{ [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 initial conditions with zero angular momentum 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 three-body problems. As will be briefly discussed below, the only singularities in the three-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 three-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.

The corresponding series, however, 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 makes it possible 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-angular-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. Using the theory of random walks, the probability of different outcomes may be computed.^{ [20] }^{ [21] }

The gravitational problem of three bodies in its traditional sense dates in substance from 1687, when Isaac Newton published his * 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 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 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.^{ [22] } 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.^{ [23] }

George William Hill worked on the restricted problem in the late 19th century.^{ [24] }

In 2019, Breen et al. announced a fast neural network solver for the three-body problem, trained using a numerical integrator.^{ [25] }

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.^{ [26] }

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.^{ [27] } 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.^{ [27] }^{ [28] }

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.^{ [29] }

The three-body problem is a special case of the n-body problem, which describes how n objects 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;^{ [30] } 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.

In the classic 1951 science-fiction film * The Day the Earth Stood Still *, the alien Klaatu, using the pseudonym Mr. Carpenter, makes some annotations to equations on Prof. Barnhardt's blackboard. Those equations are an accurate description of a particular form of the three-body problem.

The first volume of Chinese author Liu Cixin's * Remembrance of Earth's Past * trilogy is titled * The Three-Body Problem * and features the three-body problem as a central plot device.^{ [31] }

In physics, **angular momentum** is the rotational analog 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. Angular momentum has both a direction and a magnitude, and both are conserved. Bicycles and motorcycles, frisbees rifled bullets, and gyroscopes owe their useful properties to conservation of angular momentum. Conservation of angular momentum is also why hurricanes form spirals and neutron stars have high rotational rates. In general, conservation limits the possible motion of a system, but it does not uniquely determine it.

**Mass** is the quantity of matter in a physical body. It is also a measure of the body's inertia, the resistance to acceleration when a net force is applied. An object's mass also determines the strength of its gravitational attraction to other bodies.

In celestial mechanics, an **orbit** is the curved trajectory of an object such as the trajectory of a planet around a star, or of a natural satellite around a planet, or of an artificial satellite around an object or position in space such as a planet, moon, asteroid, or Lagrange point. 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 governs the wave 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 **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.

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 binary star or 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.

The **Boltzmann equation** or **Boltzmann transport equation** (**BTE**) describes the statistical behaviour of a thermodynamic system not in a state of equilibrium, devised by Ludwig Boltzmann in 1872. The classic example of such a system is a fluid with temperature gradients in space causing heat to flow from hotter regions to colder ones, by the random but biased transport of the particles making up that fluid. In the modern literature the term Boltzmann equation is often used in a more general sense, referring to any kinetic equation that describes the change of a macroscopic quantity in a thermodynamic system, such as energy, charge or particle number.

A **classical field theory** is a physical theory that predicts how one or more physical fields interact with matter through **field equations**, without considering effects of quantization; theories that incorporate quantum mechanics are called quantum field theories. In most contexts, 'classical field theory' is specifically meant to describe electromagnetism and gravitation, two of the fundamental forces of nature.

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 due to additional factors like time and space distortions.

**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 Society. pp. 8–12. Bibcode:1997ptbp.book.....B. ISBN 978-0-8218-0367-7. - ↑ "The Three-Body Problem" (PDF).
- 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".
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- ↑ 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. S2CID 10024592. - ↑ 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. S2CID 84838204. - ↑ 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.
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(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. S2CID 89615142. - ↑ Technion (6 October 2021). "A Centuries-Old Physics Mystery? Solved".
*SciTechDaily*. SciTech . Retrieved 12 October 2021. - ↑ Ginat, Yonadav Barry; Perets, Hagai B. (23 July 2021). "Analytical, Statistical Approximate Solution of Dissipative and Nondissipative Binary-Single Stellar Encounters".
*Physical Review*.**11**(3): 031020. arXiv: 2011.00010 . doi:10.1103/PhysRevX.11.031020. S2CID 235485570 . Retrieved 12 October 2021. - ↑ 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.
- ↑ "Coplanar Motion of Two Planets, One Having a Zero Mass". Annals of Mathematics, Vol. III, pp. 65–73, 1887.
- ↑ 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. S2CID 204734498.
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*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".
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*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.

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