Constraints to the semimajor axis of outer particles with nodal librations by general relativity effects

TL;DR

This paper analytically investigates how general relativity influences the semimajor axis limits for outer particles undergoing nodal librations in a three-body system, revealing key dependencies on system parameters.

Contribution

It provides the first analytical derivation of the maximum semimajor axis for outer particles experiencing nodal librations considering GR effects, validated by N-body simulations.

Findings

GR effects set an upper limit on the semimajor axis for librating particles

The limit depends on star and planet masses, and orbital eccentricities

N-body simulations confirm the analytical criteria

Abstract

We study nodal librations of outer particles in the framework of the elliptical restricted three-body problem including general relativity (GR) effects. From an analytical treatment based on secular interactions up to quadrupole level, we derive equations that define the nodal libration region of an outer test particle, which depends on the physical and orbital parameters of the bodies of the system. From this, we analyze how the GR constrains the semimajor axis of outer test particles that experience nodal librations under the effects of an inner planet around a single stellar component. Such an upper limit of the semimajor axis, which is called a2,lim , depends on the mass of the star ms, the mass m1, the semimajor axis a1, and the eccentricity e1 of the inner planet, and the eccentricity e2 of the outer test particle. On the one hand, our results show that the greater m1, a1, and e2 and the smaller ms, the greater the value of a2,lim. On the other hand, for fixed ms, m1, a1, and e2, a2,lim does not strongly depend on e1, except for large values of such an orbital parameter. We remark that N-body experiments of particular scenarios that include GR show results consistent with the analytical criteria derived in the present research. Moreover, the study of hypothetical small body populations of real systems composed of a single star and an inner planetary-mass companion show that the GR effects can play a very important role in their global dynamics.