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Jupiter's atmosphere is enriched in C, N, S, P, Ar, Kr and Xe with respect tosolar abundances by a factor of ~3. Gas Giant envelopes are mainly enrichedthrough the dissolution of solids in the atmosphere, and this constantenrichment factor is puzzling since several of the above elements are notexpected to have been in the solid phase in Jupiter's feeding zone; mostseriously, Ar and the main carrier of N, N2, only condense at the very lowtemperatures, 21-26 K, associated with the outer solar nebula. We propose thata plausible solution to the enigma of Jupiter's uniform enrichment pattern isthat Jupiter's core formed exterior to the N2 and Ar snowlines, beyond 30 au,resulting in a Solar composition core in all volatiles heavier than Ne. Duringenvelope accretion and planetesimal bombardment, some of the core mixed in withthe envelope causing the observed enrichment pattern. We show that thisscenario naturally produces the observed atmosphere composition, even withsubstantial pollution from N-poor pebble and planetesimal accretion inJupiter's final feeding zone. We note that giant core formation at largenebular radii is consistent with recent models of gas giant core formationthrough pebble accretion, which requires the core to form exterior to Jupiter'scurrent location to counter rapid inward migration during the core and envelopeformation process. If this scenario is common, gas giant core formation mayaccount for many of the gaps observed in protoplanetary disks between 10s and100 au.

Jupiter's composition suggests its core assembled exterior to the N2 snowline