Abstract

In the present work the geodesic equation represents the equations of motion of the particles along the geodesics is derived. The deviation of the curved space-time metric tensor from that of the Minkowski tensor is considered as a perturbation. The quantities is expanded in powers of c-2. The equations of motion of the relativistic three body problem in the PN formalism are obtained.

Highlights

  • The Three body problem concerns with the motion of a small particle of negligible mass moving under the gravitational influence of two massive objects m1 and m2

  • In 1772, Euler [5] first introduced a synodic coordinate system, the use of which led to an integral of the equations of motion, known today as the Jacobian integral

  • Euler himself did not discover the Jacobia integral which was first given by Jacobi [1] who, as Wintner remarks, “rediscovered” the synodic system

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Summary

Introduction

The Three body problem concerns with the motion of a small particle of negligible mass moving under the gravitational influence of two massive objects m1 and m2. It’s history began with Euler and Lagrange continues with Jacobi [1], Hill [2], Poincaré [3], and Birkhoff [4]. In 1772, Euler [5] first introduced a synodic (rotating) coordinate system, the use of which led to an integral of the equations of motion, known today as the Jacobian integral. Euler himself did not discover the Jacobia integral which was first given by Jacobi [1] who, as Wintner remarks, “rediscovered” the synodic system. The actual situation is somewhat complex since Jacobia published his integral in a sideral (fixed) system in which its significance is definitely less than in the synodic system.

Expansion Dimensionless Parameter
The Geodesic Equation
The Metric Tensor
Einstein Field Equations
The Ricci Tensor R
The Energy-Momentum Tensor T
The Equations of Motion of Restricted Three-Body Problem
The Restricted Three-Body Problem Notations
10. Conclusions
11. References

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