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The relationship between the compositions of giant planets and their hoststars is of fundamental interest in understanding planet formation. The solarsystem giant planets are enhanced above solar composition in metals, both intheir visible atmospheres and bulk compositions. A key question is whether themetal enrichment of giant exoplanets is correlated with that of their hoststars. Thorngren et al. (2016) showed that in cool (Teq < 1000 K) giantexoplanets, the total heavy-element mass increases with total Mp and the heavyelement enrichment relative to the parent star decreases with total Mp. Intheir work, the host star metallicity was derived from literature [Fe/H]measurements. Here we conduct a more detailed and uniform study to determinewhether different host star metals (C, O, Mg, Si, Fe, and Ni) correlate withthe bulk metallicity of their planets, using correlation tests and Bayesianlinear fits. We present new host star abundances of 19 cool giant planetsystems, and combine these with existing host star data for a total of 22 coolgiant planet systems (24 planets). Surprisingly, we find no clear correlationbetween stellar metallicity and planetary residual metallicity (the relativeamount of metal versus that expected from the planet mass alone), which is inconflict with common predictions from formation models. We also find apotential correlation between residual planet metals and stellarvolatile-to-refractory element ratios. These results provide intriguing newrelationships between giant planet and host star compositions for futuremodeling studies of planet formation.

Do Metal-Rich Stars Make Metal-Rich Planets? New Insights on Giant Planet Formation from Host Star Abundances