  Many observed giant planets lie on eccentric orbits. Such orbits could be the
result of strong scatterings with other giant planets. The same dynamical
instability that produces these scatterings may also cause habitable planets in
interior orbits to become ejected, destroyed, or be transported out of the
habitable zone. We say that a habitable planet has resilient habitability if it
is able to avoid ejections and collisions and its orbit remains inside the
habitable zone. Here we model the orbital evolution of rocky planets in
planetary systems where giant planets become dynamically unstable. We measure
the resilience of habitable planets as a function of the observed, present-day
masses and orbits of the giant planets. We find that the survival rate of
habitable planets depends strongly on the giant planet architecture. Equal-mass
planetary systems are far more destructive than systems with giant planets of
unequal masses. We also establish a link with observation; we find that giant
planets with present-day eccentricities higher than 0.4 almost never have a
habitable interior planet. For a giant planet with an present-day eccentricity
of 0.2 and semimajor axis of 5 AU orbiting a Sun-like star, 50% of the orbits
in the habitable zone are resilient to the instability. As semimajor axis
increases and eccentricity decreases, a higher fraction of habitable planets
survive and remain habitable. However, if the habitable planet has rocky
siblings, there is a significant risk of rocky planet collisions that would
sterilize the planet.
