  Jupiter played an important role in determining the structure and
configuration of the Solar System. Whereas hot-Jupiter type exoplanets
preferentially form around metal-rich stars, the conditions required for the
formation of planets with masses, orbits and eccentricities comparable to
Jupiter (Jupiter analogues) are unknown. Using spectroscopic metallicities, we
show that stars hosting Jupiter analogues have an average metallicity close to
solar, in contrast to their hot-Jupiter and eccentric cool Jupiter
counterparts, which orbit stars with super-solar metallicities. Furthermore,
the eccentricities of Jupiter analogues increase with host star metallicity,
suggesting that planet-planet scatterings producing highly eccentric cool
Jupiters could be more common in metal-rich environments. To investigate a
possible explanation for these metallicity trends, we compare the observations
to numerical simulations, which indicate that metal-rich stars typically form
multiple Jupiters, leading to planet-planet interactions and, hence, a
prevalence of either eccentric cool Jupiters or hot-Jupiters with circularized
orbits. Although the samples are small and exhibit variations in their
metallicities, suggesting that numerous processes other than metallicity affect
the formation of planetary systems, the data in hand suggests that Jupiter
analogues and terrestrial-sized planets form around stars with average
metallicities close to solar, whereas high metallicity systems preferentially
host eccentric cool Jupiter or hot-Jupiters, indicating higher metallicity
systems may not be favorable for the formation of planetary systems akin to the
Solar System.
