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Jupiter played an important role in determining the structure andconfiguration of the Solar System. Whereas hot-Jupiter type exoplanetspreferentially form around metal-rich stars, the conditions required for theformation of planets with masses, orbits and eccentricities comparable toJupiter (Jupiter analogues) are unknown. Using spectroscopic metallicities, weshow that stars hosting Jupiter analogues have an average metallicity close tosolar, in contrast to their hot-Jupiter and eccentric cool Jupitercounterparts, 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 coolJupiters could be more common in metal-rich environments. To investigate apossible explanation for these metallicity trends, we compare the observationsto numerical simulations, which indicate that metal-rich stars typically formmultiple Jupiters, leading to planet-planet interactions and, hence, aprevalence of either eccentric cool Jupiters or hot-Jupiters with circularizedorbits. Although the samples are small and exhibit variations in theirmetallicities, suggesting that numerous processes other than metallicity affectthe formation of planetary systems, the data in hand suggests that Jupiteranalogues and terrestrial-sized planets form around stars with averagemetallicities close to solar, whereas high metallicity systems preferentiallyhost eccentric cool Jupiter or hot-Jupiters, indicating higher metallicitysystems may not be favorable for the formation of planetary systems akin to theSolar System.

Jupiter Analogues Orbit Stars with an Average Metallicity Close to that of the Sun