# Simulations of the dynamics of the debris disks in the systems Kepler-16, Kepler-34, and Kepler-35

## TL;DR

This study models the long-term behavior of debris disks in binary star systems Kepler-16, Kepler-34, and Kepler-35, revealing conditions for stable coorbital rings and implications for planet detection.

## Contribution

It provides new insights into the formation of stable coorbital rings in binary systems and their observational signatures, based on detailed dynamical simulations.

## Key findings

- Stable coorbital rings form in Kepler-16 and Kepler-35.
- High eccentricities in Kepler-34 inhibit ring formation.
- Detection of circumbinary structures can indicate the presence of planets.

## Abstract

The long-term dynamics of planetesimals in debris discs in models with parameters of binary star systems Kepler-16, Kepler-34 and Kepler-35 with planets is investigated. Our calculations have shown the formation of a stable coorbital with the planet ring is possible for Kepler-16 and Kepler-35 systems. In Kepler-34 system, significant eccentricities of the orbits of the binary and planets can to prevent the formation of such a structure. Detection circumbinary annular structures in observations of systems binary stars can be evidence of the existence of planets, retaining coorbital rings from dust and planetesimals.