  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.
