# Jupiter's formation in the vicinity of the amorphous ice snowline

## TL;DR

This study models how inward drifting amorphous ice particles with volatiles could enrich Jupiter's atmosphere, explaining observed volatile levels and supporting various formation scenarios within a few million years and within 20 AU of the Sun.

## Contribution

It demonstrates that accretion of supersolar nebular gas enriched by amorphous ice particles can account for Jupiter's volatile enrichments, aligning with multiple formation models.

## Key findings

- Jupiter's volatile enrichments can be explained by inward drifting amorphous ice particles.
- Jupiter's envelope could have accreted gas with metallicity similar to current measurements.
- Formation likely occurred within 0.5--2 Myr and 0.5--20 AU from the Sun.

## Abstract

Argon, krypton, xenon, carbon, nitrogen, sulfur, and phosphorus have all been measured enriched by a quasi uniform factor in the 2--4 range, compared to their protosolar values, in the atmosphere of Jupiter. To elucidate the origin of these volatile enrichments, we investigate the possibility of inward drift of particles made of amorphous ice and adsorbed volatiles, and their ability to enrich in heavy elements the gas phase of the protosolar nebula once they cross the amorphous-to-crystalline ice transition zone, following the original idea formulated by Monga & Desch (2015). To do so, we use a simple accretion disk model coupled to modules depicting the radial evolution of icy particles and vapors, assuming growth, fragmentation and crystallization of amorphous grains. We show that it is possible to accrete supersolar gas from the nebula onto proto-Jupiter's core to form its envelope, and allowing it to match the observed volatile enrichments. Our calculations suggest that nebular gas with a metallicity similar to that measured in Jupiter can be accreted by its envelope if the planet formed in the $\sim$0.5--2 Myr time range and in the 0.5--20 AU distance range from the Sun, depending on the adopted viscosity parameter of the disk. These values match a wide range of Jupiter's formation scenarios, including in situ formation and migration/formation models.