Stable Orbits in the Feeding Zone of the Planet Proxima Centauri c

TL;DR

This study models the orbital evolution of planetesimals around Proxima Centauri c over a billion years, identifying stable and resonant orbits within its feeding zone.

Contribution

It provides new insights into the long-term orbital stability and resonance behavior of planetesimals near Proxima Centauri c, based on extensive orbital simulations.

Findings

Some planetesimals remain in stable orbits within the feeding zone.

Resonances such as 1:1, 5:4, and 3:4 are common among stable planetesimals.

Chaotic orbits can evolve into long-term resonant states.

Abstract

Estimates of the size of the feeding zone of the planet Proxima Centauri c have been made at initial orbital eccentricities of planetesimals equal to 0.02 or 0.15. The research is based on the results of modeling of the evolution of planetesimals' orbits under the influence of the star and planets Proxima Centauri c and b. The considered time interval reached a billion years. It was found that after the accumulation of the planet Proxima Centauri c some planetesimals may have continues to move in stable elliptical orbits within its feeding zone, largely cleared of planetesimals. Usually such planetesimals can move in some resonances with the planet (Proxima Centauri c), for example, in the resonance 1:1 (as Jupiter Trojans), 5:4 and 3:4 and usually have small eccentricities. Some planetesimals that moved for a long time (1-2 million years) along chaotic orbits fell into the resonances 5:2 and 3:10 with the planet Proxima Centauri c and moved in them at least tens of millions of years.