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Many observed giant planets lie on eccentric orbits. Such orbits could be theresult of strong scatterings with other giant planets. The same dynamicalinstability that produces these scatterings may also cause habitable planets ininterior orbits to become ejected, destroyed, or be transported out of thehabitable zone. We say that a habitable planet has resilient habitability if itis able to avoid ejections and collisions and its orbit remains inside thehabitable zone. Here we model the orbital evolution of rocky planets inplanetary systems where giant planets become dynamically unstable. We measurethe resilience of habitable planets as a function of the observed, present-daymasses and orbits of the giant planets. We find that the survival rate ofhabitable planets depends strongly on the giant planet architecture. Equal-massplanetary systems are far more destructive than systems with giant planets ofunequal masses. We also establish a link with observation; we find that giantplanets with present-day eccentricities higher than 0.4 almost never have ahabitable interior planet. For a giant planet with an present-day eccentricityof 0.2 and semimajor axis of 5 AU orbiting a Sun-like star, 50% of the orbitsin the habitable zone are resilient to the instability. As semimajor axisincreases and eccentricity decreases, a higher fraction of habitable planetssurvive and remain habitable. However, if the habitable planet has rockysiblings, there is a significant risk of rocky planet collisions that wouldsterilize the planet.

Survival of habitable planets in unstable planetary systems