  The dynamics of the Restricted 3 Body Problem in the Post Newtonian context
have been, and continue to be, studied extensively and a number of
characteristics such as ejections of bodies from the system, precession of
orbits, chaotic trajectories and collisions are investigated and classified. In
this paper, I examine the extent to which these characteristics are
attributable to Relativistic causes (more correctly Post Newtonian
approximations of Relativistic causes) or more prosaically whether these
characteristics already exist in the Newtonian case and whether these or other
effects would also be caused by the time of propagation of the field, the
impact of which is less well covered in the literature. In this project I have
written bespoke code for the simulations and present the results in a
methodical way showing many of the steps in the process. In the Appendices, I
discuss the technical challenges of constructing, testing and calibrating the
code, so that other non-experts in the field can reproduce the code and results
and build on the work that I have done. Although the work done here must be
considered preliminary, results suggest that the impact of the field
propagation time on the behaviour of the test mass in the restricted 3 body
problem outweighs the impact of the Post Newtonian corrections, in particular
due to a transfer of angular momentum from the binary system to the test mass,
and this effect may therefore be of interests to those studying accretion discs
of binary systems.
