A Review on Co-orbital Motion in Restricted and Planetary Three-body Problems |
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| Institution: | 1. School of Astronomy and Space Science, Nanjing University, Nanjing 210023 China;2. Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030 China;1. National Time Service Center, Chinese Academy of Sciences, Xi’an 710600;2. School of Electronic Electrical and Communication Engineering, University of Chinese Academy of Sciences, Beijing 100049;3. Key Laboratory of Precise Positioning and Timing Technology, Chinese Academy of Sciences, Xi’an 710600;4. Key Laboratory of Time and Frequency Primary Standards, Chinese Academy of Sciences, Xi’an 710600;1. School of Health Science and Engineering, University of Shanghai for Science and Technology, Shanghai 200093;2. Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030;3. Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Nanjing 210023;4. Shanghai Key Laboratory of Space Navigation and Position Techniques, Shanghai 20003;1. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023;2. School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026;1. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023;2. School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026;3. Key Laboratory of Planetary Sciences, Chinese Academy of Sciences, Nanjing 210023;1. Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011 China;2. Xinjiang Key Laboratory of Microwave Technology, Urumqi 830011 China;3. School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing 100049 China |
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| Abstract: | The 1:1 mean motion resonance may be referred to as the lowest order mean motion resonance in restricted or planetary three-body problems. The five well-known libration points of the circular restricted three-body problem are five equilibriums of the 1:1 resonance. Coorbital motion may take different shapes of trajectory. In case of small orbital eccentricities and inclinations, tadpole-shape and horseshoe-shape orbits are well-known. Other 1:1 libration modes different from the elementary ones can exist at moderate or large eccentricities and inclinations. Coorbital objects are not rare in our solar system, for example the Trojans asteroids and the coorbital satellite systems of Saturn. Recently, dozens of coorbital bodies have been identified among the near-Earth asteroids. These coorbital asteroids are believed to transit recurrently between different 1:1 libration modes mainly due to orbital precessions, planetary perturbations, and other possible effects. The Hamiltonian system and the Hill’s three-body problem are two effective approaches to study coorbital motions. To apply the perturbation theory to the Hamiltonian system, standard procedures involve the development of the disturbing function, averaging and normalization, theory of ideal resonance model, secular perturbation theory, etc. Global dynamics of coorbital motion can be revealed by the Hamiltonian approach with a suitable expansion. The Hill’s problem is particularly suitable for the studies on the relative motion of two coorbital bodies during their close encounter. The Hill’s equation derived from the circular restricted three-body problem is well known. However, the general Hill’s problem whose equation of motion takes exactly the same form applies to the non-restricted case where the mass of each body is non-negligible, namely the planetary case. The Hill’s problem can be transformed into a “canonical shape” so that the averaging principle can be applied to construct a secular perturbation theory. Besides the two analytical theories, numerical methods may be consulted, for example the approach of periodic orbit, the surface of section, and the computation of invariant manifolds carried by equilibriums or periodic orbits. |
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