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Approximately half of the planets discovered by NASA's Kepler mission are insystems where just a single planet transits its host star, and the remainingplanets are observed to be in multi-planet systems. Recent analyses havereported a dichotomy in the eccentricity distribution displayed by systemswhere a single planet transits compared with that displayed by the multi-planetsystems. Using $N$-body simulations, we examine the hypothesis that thisdichotomy has arisen because inner systems of super-Earths are frequentlyaccompanied by outer systems of giant planets that can become dynamicallyunstable and perturb the inner systems. Our initial conditions are constructedusing a subset of the known Kepler five-planet systems as templates for theinner systems, and systems of outer giant planets with masses between those ofNeptune and Saturn that are centred on orbital radii $2 \le a_{\rm p} \le 10$au. The parameters of the outer systems are chosen so that they are alwaysbelow an assumed radial velocity detection threshold of 3 ms$^{-1}$. Theresults show an inverse relation between the mean eccentricities and themultiplicites of the systems. Performing synthetic transit observation of thefinal systems reveals dichotomies in both the eccentricity and multiplicitydistributions that are close to being in agreement with the Kepler data. Hence,understanding the observed orbital and physical properties of the compactsystems of super-Earths discovered by Kepler may require holistic modellingthat couples the dynamics of both inner and outer systems of planets during andafter the epoch of formation.

On the origin of the eccentricity dichotomy displayed by compact super-Earths: dynamical heating by cold giants