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The two innermost planets of the Proxima Centauri system are separated byjust 0.02 au, inducing strong gravitational interactions between them. Weassess this interaction by leveraging fast orbital stability indicators andfind that orbital stability is very likely if the initial eccentricities ofplanets b and d are less than $\sim 0.2$, but cannot confirm stability atlarger values. We find that stability is not strongly affected by the truemasses of the planets or by the distant planet c. However, mutual inclinationsbetween 95$^\circ$ and 142$^\circ$ often result in unstable motion. We furtherexplore the long-term evolution of the orbits in these stable regions ofparameter space and find that circularization can take over 5 Gyr. This tidalevolution could support surface energy fluxes in excess of 1 W m$^{-2}$ forover 1 Gyr, possibly affecting planet b's habitability.

Orbital Stability and Secular Dynamics of the Proxima Centauri Planetary System