Abstract
General properties of the three-body problem in a model of modified dynamics are investigated. It is shown that the three-body problem in this model shares some characters with the similar problem in Newtonian dynamics. Moreover, the planar restricted three-body problem is solved analytically for this type of extended gravity and it is proved that under certain conditions, which generally happen at galactic and extragalactic scales, the orbits around \(L_{4}\) and \(L_{5}\) Lagrange points are stable. Furthermore, a code is provided to compare the behavior of orbits in the restricted three-body problem under Newtonian and modified dynamics. Orbit integrations based on this code show contrasting orbital behavior under the two dynamics and specially exhibit in a qualitative way that the rate of ejections is smaller in the modified dynamics compared to Newtonian gravity. These results could help us to search for observational signatures of extended gravities.
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Acknowledgements
I would like to thank Ramezan Ebrahimi for checking the equations in Sec. 3. Also, I appreciate fruitful discussions with members of the astronomy and astrophysics group, Ferdowsi University of Mashhad. I appreciate helpful discussions with Elham Nazari on the nature of the problem of the binary systems. In addition, I benefited from comments and suggestions by the reviewers for which I am very grateful. (One comment helped me to find an error in Fig. 1 of the earlier version of this manuscript.) This research has made use of NASA’s Astrophysics Data System. The MATHEMATICA codes related to orbit integration are provided in my GitHub repository (https://github.com/Shenavar/ThreeBodyinMOD).
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Shenavar, H. Three-body problem in modified dynamics. Celest Mech Dyn Astron 135, 19 (2023). https://doi.org/10.1007/s10569-023-10137-4
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DOI: https://doi.org/10.1007/s10569-023-10137-4