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The imprints of stellar nucleosynthesis and chemical evolution of the galaxycan be seen in different stellar populations, with older generation starsshowing higher $\alpha$-element abundances while the later generations becomingenriched with iron-peak elements. The evolutionary connections and chemicalcharacteristics of circumstellar disks, stars, and their planetary companionscan be inferred by studying the interdependence of planetary and host starproperties. Numerous studies in the past have confirmed that high-mass giantplanets are commonly found around metal-rich stars, while the stellar hosts oflow-mass planets have a wide range of metallicity. In this work, we analyzedthe detailed chemical abundances for a sample of $>900$ exoplanet hosting starsdrawn from different radial velocity and transit surveys. We correlate thestellar abundance trends for $\alpha$ and iron-peak elements with the planets'mass. We find the planet mass-abundance correlation to be primarily negativefor $\alpha$-elements and marginally positive or zero for the iron-peakelements, indicating that stars hosting giant planets are relatively younger.This is further validated by the age of the host stars obtained from isochronefitting. The later enrichment of protoplanetary material with iron andiron-peak elements is also consistent with the formation of the giant planetsvia the core accretion process. A higher metal fraction in the protoplanetarydisk is conducive to rapid core growth, thus providing a plausible route forthe formation of giant planets. This study, therefore, indicates the observedtrends in stellar abundances and planet mass are most likely a naturalconsequence of Galactic chemical evolution.

Galactic chemical evolution of exoplanet host stars: Are high-mass planetary systems young?