Compact planetary systems perturbed by an inclined companion: I. Vectorial representation of the secular model

TL;DR

This paper introduces a vectorial approach to modeling the secular dynamics of compact planetary systems, simplifying calculations and enabling analysis of large tilts and complex interactions.

Contribution

The paper presents a new vectorial formulation of the secular model that simplifies calculations and handles large tilts in planetary systems.

Findings

Vectorial expressions are simpler than traditional elliptical element formulations.

The model can handle arbitrary eccentricities and inclinations.

Applications include solar system oscillations and exoplanet Kozai cycles.

Abstract

The non-resonant secular dynamics of compact planetary systems are modeled by a perturbing function which is usually expanded in eccentricity and absolute inclination with respect to the invariant plane. Here, the expressions are given in a vectorial form which naturally leads to an expansion in eccentricity and mutual inclination. The two approaches are equivalent in most cases, but the vectorial one is specially designed for those where a quasi-coplanar system tilts as a whole by a large amount. Moreover, the vectorial expressions of the Hamiltonian and of the equations of motion are slightly simpler than those given in terms of the usual elliptical elements. We also provide the secular perturbing function in vectorial form expanded in semimajor axis ratio allowing for arbitrary eccentricities and inclinations. The interaction between the equatorial bulge of a central star and its planets is also provided, as is the relativistic periapse precession of any planet induced by the central star. We illustrate the use of this representation for following the secular oscillations of the terrestrial planets of the solar system, and for Kozai cycles as may take place in exoplanetary systems.