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Recent observations of extrasolar gas giants suggest super-stellar C/O ratiosin planetary atmospheres, while interior models of observed extrasolar giantplanets additionally suggest high heavy element contents. Furthermore, recentobservations of protoplanetary disks revealed super-solar C/H ratios, which areexplained by inward drifting and evaporating pebbles, enhancing the volatilecontent of the disk. We investigate how the inward drift and evaporation ofvolatile rich pebbles influences the atmospheric C/O ratio and heavy elementcontent of giant planets growing by pebble and gas accretion. To achieve thisgoal, we perform semi analytical 1D models of protoplanetary disks includingthe treatment of viscous evolution and heating, pebble drift and simplechemistry to simulate the growth of planets from planetary embryos to Jupitermass objects by accretion of pebbles and gas while they migrate through thedisk. Our simulations show that the composition of the planetary gas atmosphereis dominated by the accretion of vapour, originating from inward driftingevaporating pebbles. This process allows the giant planets to harbour largeheavy element contents. In addition, our model reveals that giant planetsoriginating further away from the central star have a higher C/O ratio onaverage due to the evaporation of methane rich pebbles in the outer disk. Theseplanets can then also harbour super-solar C/O ratios, in line with exoplanetobservations. However, planets formed in the outer disk harbour a smaller heavyelement content, due to a smaller vapour enrichment of the outer disk. Ourmodel predicts that giant planets with low/large atmospheric C/O should harboura large/low total heavy element content. We further conclude that the inclusionof pebble evaporation at evaporation lines is a key ingredient to determine theheavy element content and composition of giant planets.

How drifting and evaporating pebbles shape giant planets I: Heavy element content and atmospheric C/O