Three-body problem has two distinguishable meanings:

1. In an extended modern sense, a three-body problem is a class of problems in classical or quantum mechanics that model the motion of three particles. Typically, all three particles are considered as point masses, neglecting their shape and internal structure, and the interaction among them is a scalar potential such as gravity or electromagnetism.^{[citation needed]}
2. The three-body problem, in its traditional sense, is (generically) the problem of taking an initial set of data that specifies directly or indirectly the positions, masses, and velocities of three bodies, for some particular point in time, and then using that set of data to determine the motions of the three bodies, and to find their positions at other times, in accordance with the laws of classical mechanics: Newton's laws of motion and of universal gravitation. 'Solving' this problem means providing a generally applicable method for making this kind of determination of gravitational trajectories, or possessing such a method.

Historically, the first specific three-body problem to receive extended study was the one involving the Moon, the Earth and the Sun.

Contents 1 History 2 Non-relativistic movement 3 Examples 4 Classical versus quantum mechanics 5 n-body problem 6 Notes 7 See also 8 References 9 External Links

[edit] History

The gravitational problem of three bodies in its traditional sense dates in substance from 1687, when Isaac Newton published his 'Principia' (Philosophiae 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.

It was later on that the problem gained special fame (among other reasons, for its great difficulty) under the specific name of the three-body problem.

During the second quarter of the eighteenth century, the problem of improving the accuracy of the lunar theory came to be of topical interest. The topicality arose mainly because it was perceived that the results should be applicable to navigation, that is, to the development of a method for determining geographical longitude at sea. Following Newton's work, it was appreciated that at least a major part of the problem in lunar theory consisted in evaluating the perturbing effect of the Sun on the motion of the Moon around the Earth.

Jean d'Alembert and Alexis Clairaut, who developed a longstanding rivalry, both attempted to analyze the problem in some degree of generality, and by the use of differential equations to be solved by successive approximations. They submitted their competing first analyses to the Academie Royale des Sciences in 1747.^[1]

It was in connection with these researches, in Paris, in the 1740s, that the name "three-body problem" (Problème des Trois Corps) began to be commonly used. An account published in 1761 by Jean d'Alembert indicates that the name was first used in 1747.^[2]

[edit] Non-relativistic movement

The energy E of movement is assumed to be small compared to their mass, allowing one to describe the bodies with non-relativistic mechanics. This implies that all the movement refers to velocities small compared to the speed of light c.^{[citation needed]}

In classical mechanics, movement with higher velocities causes the radiation of gravitational waves, and the system cannot be considered as conservative.^{[citation needed]}

In quantum mechanics, in addition, at high speed, the creation and annihilation of particles becomes possible, so, it is not possible to keep the number of particles constant.^{[citation needed]}

In such a way, the 3-body problem is a certain class of approximations.

[edit] Examples

Due to the small value of the fine-structure constant, various atomic systems can be described as 3-body systems:^{[citation needed]} Atoms of helium or the helium-like ions for example; however, at high atomic numbers, the velocities become relativistic and consequently the approximation becomes inaccurate.

In the case of the helium atom or helium-like ions, the system is determined by the mass of the nucleus, mass of the electron, and the Coulomb interaction between them.^{[citation needed]}

In addition, some properties of simple molecules can be described, assuming the fast movement of electrons (which are many orders of magnitude lighter than nuclei); then, the electrons determine some effective potential, and the movement of atoms can be described with this potential. In this sense, the 3-atomic molecule (for example, water, or the carbon dioxide) can be treated as a 3-body problem.^{[citation needed]} This description is valid at weak excitations (for example, at room temperature), and can be used for estimating the thermal capacities of gases; the crucial thing to determine is, how many vibrational degrees of freedom are excited at a given temperature.^{[citation needed]}

In the 21st century, experiments with atomic traps and molecular traps enhance the possibilities to deal with 3-body systems.^{[citation needed]}

Upon excitation with short pulses, during the short time after the excitation, such systems may show trajectories and other attributes typical of classical mechanics.^{[citation needed]}

Another example of a classical 3-body problem is the movement of a planet with a satellite around a star. In most cases such a system can be factorized, considering the movement of the complex (planet and satellite) around a star as a single particle; then, considering the movement of the satellite around the planet, neglecting the movement around the star. In this case, the problem is simplified to the 2-body problem. However, the effect of the star on the movement of the satellite around the planet can be considered as a perturbation.

[edit] Classical versus quantum mechanics

Physicist Vladimir Krivchenkov used the 3-body problem as an example, showing the simplicity of quantum mechanics in comparison to classical mechanics. The quantum 3-body problem is studied in university courses of quantum mechanics;^[3] in particular, the energy of the ground state and the first excited states can be estimated by hand, even without the use of computers, using perturbation theory.^{[citation needed]} As for classical mechanics, the variety of divergent trajectories with various Lyapunov exponents^{[citation needed]} makes the problem too difficult for undergraduate courses.

The 3-body problem is also used to establish the deterministic interpretation of quantum mechanics.^{[citation needed]} According to this concept, quantum mechanics is a completely deterministic science (compare to the Copenhagen interpretation). No probability is necessary for the description of a closed system: there are no trajectories, and therefore there are no divergent trajectories, which would require the stochastic description. However, probability appears when the system, or its parts, are so complicated that we need to apply classical mechanics for the solution.^{[citation needed]}

The 3-body system is the simplest mechanical system that allows for unstable trajectories and therefore probability, in the case of classical mechanics. In the case of gravitating masses, one of the questions of the 3-body problem is: For some given class of initial conditions, what is the probability that during some time t, two particles get close enough, providing the energy that would allow the third particle to leave the system?^{[citation needed]}

In the case of quantum mechanics, the main part of the 3-body problem refers to the finding the eigenstates and their energies.^{[citation needed]}

[edit] n-body problem

The 3-body problem is a special case of the n-body problem. N-Body problems deal with the question of how n objects will move under one of the physical forces such as gravity. These problems don’t have an analytic solution for n greater than two (Except for special cases). Thus, for these kinds of problems using numerical solutions is unavoidable. Numerical solutions simulate the N-body system using computer codes. see N-body simulation. Atomic systems (atoms, ions, 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; and the huge number of particles (stars) in such system makes the analytic ("exact") solution impossible, and statistical methods are used instead. In addition, there is uncertain information about the initial conditions for such a system. In this sense, the classical n-body problem is probabilistic. Planetary systems (star(s), planets, and their satellites) can also be treated as n-body systems. However, trajectories and analytical solutions can be constructed considering the attraction between planets as perturbation, and it is usually a good approximation.

[edit] Notes

1. ^ The 1747 memoirs of both parties can be read in the volume of 'Histoires' (including 'Memoires') of the Academie 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).

   The peculiar dating is explained by a note printed on page 390 of the 'Memoirs' section:"Even though the preceding memoirs, of Messrs. Clairaut and d'Alembert, were only read during the course of 1747, it was judged appropriate to publish them in the volume for this year" (i.e. the volume otherwise dedicated to the proceedings of 1745, but published in 1749).

2. ^ Jean 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 Mathematiques", vol.2, Paris 1761, Quatorzieme Memoire ("Reflexions sur le Probleme des trois Corps, avec de Nouvelles Tables de la Lune ...") pp.329-312, at sec.VI, p.245.
3. ^ I. I. Gol’dman and V. D. Krivchenkov. Problems in Quantum Mechanics.. 3rd ed. Mineola, N.Y.: Dover Publications, 2006. 288 pp.

[edit] See also

• N-body problem
• N-body simulation
• Galaxy formation and evolution
• Numerical methods
• Two-dimensional gas

[edit] References

Aarseth S. J., Gravitational N-Body Simulations, 2003, Cambridge University Press.

Bagla J. S., Cosmological N-body simulation: Techniques, scope and status, 2005, Current Science.

Chambers J. E., Wetherill G. W., Making the Terrestrial Planets: N-Body Integrations of Planetary Embryos in Three Dimensions, 1998, Academic Press.

Efstathiou G., Davis M., White S. D. M., Frenk C. S., Numerical techniques for large cosmological N-body simulations, 1985, ApJ.

[edit] External Links

• Applet demonstrating chaos in restricted three-body problem
• Scholarpedia description of Three Body Problem