Production of trans-Neptunian binaries through chaos-assisted capture

TL;DR

This paper analyzes how chaos-assisted capture can explain the formation of trans-Neptunian binaries, using detailed three- and four-body Hill approximations to match observed orbital distributions.

Contribution

It provides a detailed, three-dimensional analysis of chaos-assisted binary formation in the trans-Neptunian region, addressing formation rates and orbital distribution predictions.

Findings

Chaos-assisted capture explains observed binary orbit inclinations.

Predicted asymmetry between retrograde and prograde orbits.

Consistent with random distribution of mutual orbit inclinations.

Abstract

The recent discovery of binary objects in the Kuiper-belt opens an invaluable window into past and present conditions in the trans-Neptunian part of the Solar System. For example, knowledge of how these objects formed can be used to impose constraints on planetary formation theories. We have recently proposed a binary-object formation model based on the notion of chaos-assisted capture. Here we present a more detailed analysis with calculations performed in the spatial (three-dimensional) three- and four-body Hill approximations. It is assumed that the potential binary partners are initially following heliocentric Keplerian orbits and that their relative motion becomes perturbed as these objects undergo close encounters. First, the mass, velocity, and orbital element distribu- tions which favour binary formation are identified in the circular and elliptical Hill limits. We then consider intruder scattering in the circular Hill four-body problem and find that the chaos-assisted capture mechanism is consistent with observed, apparently randomly distributed, binary mutual orbit inclinations. It also predicts asymmetric distributions of retrograde versus prograde orbits. The time-delay induced by chaos on particle transport through the Hill sphere is analogous to the formation of a resonance in a chemical reaction. Implications for binary formation rates are considered and the 'fine-tuning' problem recently identified by Noll et al. (2007) is also addressed.