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Atmospheric compositions offer valuable clues to planetary formation andevolution. Jupiter has been the most well-studied giant planet in terms of itsatmosphere; however, the origin of the Jovian atmospheric composition remains apuzzle as the abundances of nitrogen and noble gases as high as those of otherelements could only originate from extremely cold environments. We propose anovel idea for explaining the Jovian atmospheric composition: Dust pileup atthe H$_2$O snow line casts a shadow and cools the Jupiter orbit so that N$_2$and noble gases can freeze. Planetesimals or a core formed in the shadowedregion can enrich nitrogen and noble gases as much as other elements throughtheir dissolution in the envelope. We compute the temperature structure of ashadowed protosolar disk with radiative transfer calculations. Then, weinvestigate the radial volatile distributions and predict the atmosphericcomposition of Jupiter with condensation calculations. We find that thevicinity of the current Jupiter orbit, approximately $3$--$7~{\rm AU}$, couldbe as cold as $30~{\rm K}$ if the small-dust surface density varies by a factorof $\gtrsim30$ across the H$_2$O snow line. According to previous grain growthsimulations, this condition could be achieved by weak disk turbulence ifsilicate grains are more fragile than icy grains. The shadow can cause thecondensation of most volatile substances, namely N$_2$ and Ar. We demonstratethat the dissolution of shadowed solids can explain the elemental abundancepatterns of the Jovian atmosphere even if proto-Jupiter was formed nearJupiter's current orbit. The disk shadow may play a vital role in controllingatmospheric compositions. The effect of the shadow also impacts theinterpretation of upcoming observations of exoplanetary atmospheres by JWST.

Jupiter's "Cold" Formation in the Protosolar Disk Shadow: An Explanation for the Planet's Uniformly Enriched Atmosphere