Choreographic solution to the general relativistic three-body problem

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dc.creatorImai, Tatsunori
dc.creatorChiba, Takamasa
dc.creatorAsada, Hideki
dc.date2007-02-14
dc.date2007-04-16
dc.date.accessioned2026-07-07T11:01:42Z
dc.date.available2026-07-07T11:01:42Z
dc.descriptionWe revisit the three-body problem in the framework of general relativity. The Newtonian N-body problem admits choreographic solutions, where a solution is called choreographic if every massive particles move periodically in a single closed orbit. One is a stable figure-eight orbit for a three-body system, which was found first by Moore (1993) and re-discovered with its existence proof by Chenciner and Montgomery (2000). In general relativity, however, the periastron shift prohibits a binary system from orbiting in a single closed curve. Therefore, it is unclear whether general relativistic effects admit a choreographic solution such as the figure eight. We carefully examine general relativistic corrections to initial conditions so that an orbit for a three-body system can be closed and a figure eight. This solution is still choreographic. This illustration suggests that the general relativistic N-body problem also may admit a certain class of choreographic solutions.
dc.description10 pages, 4 figures, text improved, accepted for publication in PRL
dc.identifierhttps://arxiv.org/abs/gr-qc/0702076
dc.identifierhttp://arxiv.org/abs/gr-qc/0702076
dc.identifierPhys.Rev.Lett.98:201102,2007
dc.identifierdoi:10.1103/PhysRevLett.98.201102
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/188031
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.subjectDynamical Systems
dc.subjectChaotic Dynamics
dc.titleChoreographic solution to the general relativistic three-body problem
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