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We present a model explaining elemental enrichments in Jupiter's atmosphere,particularly the noble gases Ar, Kr, and Xe. While He, Ne and O are depleted,seven other elements show similar enrichments ($\sim$3 times solar, relative toH). Being volatile, Ar is difficult to fractionate from ${\rm H}_{2}$. We arguethat external photoevaporation by far ultraviolet (FUV) radiation from nearbymassive stars removed ${\rm H}_{2}$, He, and Ne from the solar nebula, but Arand other species were retained because photoevaporation occurred at largeheliocentric distances where temperatures were cold enough ($\lt 30$ K) to trapthem in amorphous water ice. As the solar nebula lost H it became relativelyand uniformly enriched in other species. Our model improves on the similarmodel of Guillot \& Hueso (2006). We recognize that cold temperatures alone donot trap volatiles; continuous water vapor production also is necessary. Wedemonstrate that FUV fluxes that photoevaporated the disk generated sufficientwater vapor, in regions $\lt 30$ K, to trap gas-phase species in amorphouswater ice, in solar proportions. We find more efficient chemical fractionationin the outer disk: whereas the model of Guillot \& Hueso (2006) predicts afactor of 3 enrichment when only $< 2\%$ of the disk mass remains, we find thesame enrichments when 30\% of the disk mass remains. Finally, we predict thepresence of $\sim 0.1 \, M_{\oplus}$ of water vapor in the outer solar nebulaand in protoplanetary disks in H II regions.

External Photoevaporation of the Solar Nebula: Jupiter's Noble Gas Enrichments