Dynamical coupling of Keplerian orbits in a hierarchical four-body system: from the Galactic Centre to compact planetary systems

TL;DR

This paper investigates the long-term dynamical evolution of hierarchical four-body systems, incorporating relativistic effects and orbital eccentricities, broadening the understanding of orbital interactions from galactic centers to planetary systems.

Contribution

It extends previous models by including post-Newtonian corrections and eccentric orbits, enabling analysis of a wider range of astrophysical systems.

Findings

Post-Newtonian effects influence orbital coupling in compact systems.

Nearly coplanar orbits exhibit small inclination oscillations.

Applicable to systems from galactic centers to planetary systems.

Abstract

This study focuses on the long-term evolution of two bodies in nearby initially coplanar orbits around a central dominant body perturbed by a fourth body on a distant Keplerian orbit. Our previous works that considered this setup enforced circular orbits by adding a spherical potential of extended mass, which dampens Kozai--Lidov oscillations; it led to two qualitatively different modes of the evolution of the nearby orbits. In one scenario, their mutual interaction exceeds the effect of differential precession caused by a perturbing body. This results in a long-term coherent evolution, with nearly coplanar orbits experiencing only small oscillations of inclination. We extend the previous work by (i) considering post-Newtonian corrections to the gravity of the central body, either instead of or in addition to the potential of extended mass, (ii) relaxing the requirement of strictly circular orbits, and (iii) removing the strict requirement of complete Kozai--Lidov damping. Thus, we identify the modes of inter-orbital interaction described for the zero-eccentricity case in the more general situation, which allows for its applicability to a much broader range of astrophysical systems than considered initially. In this work, we scale the systems to the orbits of S-stars; we consider the clockwise disc to represent the perturbing body, with post-Newtonian corrections to the gravity of Sagittarius A* playing the role of damping potential. Considering post-Newtonian corrections, even stellar-mass central bodies in compact planetary systems can allow for the coupled evolution of Keplerian orbits.