  Jupiter's atmosphere is enriched in C, N, S, P, Ar, Kr and Xe with respect to
solar abundances by a factor of ~3. Gas Giant envelopes are mainly enriched
through the dissolution of solids in the atmosphere, and this constant
enrichment factor is puzzling since several of the above elements are not
expected to have been in the solid phase in Jupiter's feeding zone; most
seriously, Ar and the main carrier of N, N2, only condense at the very low
temperatures, 21-26 K, associated with the outer solar nebula. We propose that
a plausible solution to the enigma of Jupiter's uniform enrichment pattern is
that 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. During
envelope accretion and planetesimal bombardment, some of the core mixed in with
the envelope causing the observed enrichment pattern. We show that this
scenario naturally produces the observed atmosphere composition, even with
substantial pollution from N-poor pebble and planetesimal accretion in
Jupiter's final feeding zone. We note that giant core formation at large
nebular radii is consistent with recent models of gas giant core formation
through pebble accretion, which requires the core to form exterior to Jupiter's
current location to counter rapid inward migration during the core and envelope
formation process. If this scenario is common, gas giant core formation may
account for many of the gaps observed in protoplanetary disks between 10s and
100 au.
