  More than two decades ago, the Galileo probe performed in situ measurements
of the composition of Jupiter's atmosphere and found that the abundances of C,
N, S, P, Ar, Kr and Xe were all enriched by factors of 1.5--5.4 times their
protosolar value. Juno's measurements recently confirmed the supersolar N
abundance and also found that the O abundance was enriched by a factor 1--5
compared to its protosolar value. Here, we aim at determining the radial and
temporal evolution of the composition of gases and solids in the protosolar
nebula (hereafter, PSN) to assess the possibility that Jupiter's current
composition was acquired via the direct accretion of supersolar gases. To do
so, we model the evolution of a 1D $\alpha-$viscous accretion disk that
includes the radial transport of dust and ice particles and their vapors, with
their sublimation and condensation rates, to compute the composition of the
PSN. We find that the composition of Jupiter's envelope can be explained only
from its accretion from PSN gas ($\alpha \le 10^{-3}$), or from a mixture of
vapors and solids ($\alpha>10^{-3}$). The composition of the PSN at 4 AU,
namely between the locations of the H$_2$O and CO$_2$ icelines, reproduces the
one measured in Jupiter between 100 and 300 kyr of disk evolution. Our results
are found compatible with both the core accretion model, where Jupiter would
acquire its metallicity by late accretion of volatile-rich planetesimals, and
the gravitational collapse scenario, where the composition of proto-Jupiter
would be similar to that of the PSN.
