  Recent observational findings have suggested a positive correlation between
the occurrence rates of inner super-Earths and outer giant planets. These
results raise the question of whether this trend can be reproduced and
explained by planet formation theory. Here, we investigate the properties of
inner super-Earths and outer giant planets that form according to a core
accretion scenario. We study the mutual relations between these planet species
in synthetic planetary systems and compare them to the observed exoplanet
population. We invoked the Generation 3 Bern model of planet formation and
evolution to simulate 1000 multi-planet systems. We then confronted these
synthetic systems with the observed sample, taking into account the detection
bias that distorts the observed demographics. The formation of warm
super-Earths and cold Jupiters in the same system is enhanced compared to the
individual appearances, although it is weaker than what has been proposed
through observations. We attribute the discrepancy to warm and dynamically
active giant planets that frequently disrupt the inner systems, particularly in
high-metallicity environments. In general, a joint occurrence of the two planet
types requires intermediate solid reservoirs in the originating protoplanetary
disk. Furthermore, we find differences in the volatile content of planets in
different system architectures and predict that high-density super-Earths are
more likely to host an outer giant. This correlation can be tested
observationally.
