Dynamical Stability of Terrestrial Planets in the Binary {\alpha} Centauri System

TL;DR

This study assesses the stability of Earth-like planets in the habitable zones of the {\

Contribution

It introduces a new stability criterion for S-type planetary orbits in binary systems and applies it to the {\

Findings

Planetary motion in habitable zones is stable for inclinations under 40 degrees.

Orbital distance variations are similar to Earth's near the Mode I stationary solution.

The stability criterion effectively identifies regions of long-term stability.

Abstract

In this paper, we investigate whether hypothetical Earth-like planets have high probability of remaining on stable orbits inside the habitable zones around the stars A and B of {\alpha} Centauri, for lengths of time compatible with the evolution of life. We introduce a stability criterion based on the solution of the restricted three-body problem and apply it to the {\alpha} Centauri system. In this way, we determine the regions of the short-term stability of the satellite-type (S-type) planetary orbits, in both planar and three-dimensional cases. We also study the long-term stability of hypothetical planets through the dynamical mapping of the habitable zones of the stars. The topology of the maps is analyzed using the semi-analytical secular Hamiltonian model and possible processes responsible for long-lasting instabilities are identified. We verify that the planetary motion inside the habitable zones is regular, regardless of high eccentricities, for inclinations smaller than 40{\deg}. We show that the variation of the orbital distance of the planet located in the habitable zones of the binary is comparable to that of Earth, if the planet is close to the Mode I stationary solution. This result brings positive expectations for finding habitable planets in binary stars.