Papers › The Classical Gravitational N-Body Problem
The Classical Gravitational N-Body Problem
Douglas C. Heggie
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Let a number, N, of particles interact classically through Newton's Laws of Motion and Newton's inverse square Law of Gravitation. The resulting equations of motion provide an approximate mathematical model with numerous applications in astrophysics, including the motion of the moon and other bodies in the Solar System (planets, asteroids, comets and meteor particles); stars in stellar systems ranging from binary and other multiple stars to star clusters and galaxies; and the motion of dark matter particles in cosmology. For N=1 and N=2 the equations can be solved analytically. The case N=3 provides one of the richest of all unsolved dynamical problems -- the general three-body problem. For problems dominated by one massive body, as in many planetary problems, approximate methods based on perturbation expansions have been developed. In stellar dynamics, astrophysicists have developed numerous numerical and theoretical approaches to the problem for larger values of N, including treatments based on the Boltzmann equation and the Fokker-Planck equation; such N-body systems can also be modelled as self-gravitating gases, and thermodynamic insights underpin much of our qualitative understanding.
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