Long-term N-body simulations indicate that the mini-Neptune TOI 4633c is only stable over the system's 1.3 Gyr age if its orbit is retrograde relative to the highly eccentric stellar binary.
Long-Term Stability of Planets in the $\alpha$ Centauri System
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abstract
We evaluate the extent of the regions within the $\alpha$ Centauri AB star system where small planets are able to orbit for billion-year timescales, and we calculate the positions on the sky plane where planets on stable orbits about either stellar component may appear. We confirm the qualitative results of Wiegert and Holman (AJ 113, 1445, 1997) regarding the approximate size of the regions of stable orbits, which are larger for retrograde orbits relative to the binary than for prograde orbits. Additionally, we find that mean motion resonances with the binary orbit leave an imprint on the limits of orbital stability, and the effects of the Lidov-Kozai mechanism are also readily apparent.
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Planet formation and long-term stability in a very eccentric stellar binary
Long-term N-body simulations indicate that the mini-Neptune TOI 4633c is only stable over the system's 1.3 Gyr age if its orbit is retrograde relative to the highly eccentric stellar binary.