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- W86565744 abstract "After solving the one- and two-body problems, generalizing to the three-body problem should be easy, right? No! In fact, it was the gravitational three-body problem that led Henri Poincaré to discover dynamical “chaos.” Some systems are so sensitive to initial conditions that a tiny shift today can dramatically change the long-term behavior. The Solar System is actually an example: despite being well-approximated by the two-body problem, planetary motion is formally chaotic because of gravitational interactions among planets. We cannot solve the three-body problem in general, but we can gain valuable insights from two cases that are simplified but still relevant for systems ranging from satellites near Earth to planets around distant stars.KeywordsWhite DwarfWilkinson Microwave Anisotropy ProbeGravitational InteractionLagrange PointRotate Reference FrameThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves." @default.
- W86565744 created "2016-06-24" @default.
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- W86565744 date "2014-01-01" @default.
- W86565744 modified "2023-09-27" @default.
- W86565744 title "Gravitational Three-Body Problem" @default.
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- W86565744 doi "https://doi.org/10.1007/978-1-4614-9236-8_6" @default.
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