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The origin of close-in giant planets is a key open question in planetformation theory. The two leading models are (i) formation at the outer diskfollowed by migration and (ii) in situ formation. In this work we determine theatmospheric composition of warm Jupiters for both formation scenarios. Weperform N-body simulations of planetesimal accretion interior and exterior tothe water ice-line for various planetary formation locations, planetary masses,and planetesimal sizes to estimate the accreted heavy-element mass and finalplanetary composition. We find that the two models differ significantly:migrating giant planets have 2-14 times higher metallicities than planets thatform in situ. The ratio between refractories and volatiles is found to be aboveone for migrating planets but below 0.4 for planets that form in situ. We alsoidentify very different trends between heavy-element enrichment and planetarymass for these two formation mechanisms. While the metallicity of migratingplanets is found to increase with decreasing planetary mass, it is aboutconstant for in situ formation. Our study highlights the importance ofmeasuring the atmospheric composition of warm Jupiters and its connection totheir formation and evolutionary paths.

Constraining the origin of giant exoplanets via elemental abundance measurements