  We study the impact of new metallicity measurements, from solar wind data, on
the solar model. The "solar modelling problem" refers to the persisting
discrepancy between helioseismological observations and predictions of solar
models computed implementing state-of-the-art photospheric abundances. We
critically reassess the problem, in particular considering the new set of
abundances of von Steiger \& Zurbuchen 2016, determined through the \textit{in
situ} collection of solar wind samples from polar coronal holes. This new set
of abundances indicates a solar metallicity $Z_{\odot} \geq 0.0196 \pm 0.0014$,
significantly higher than the currently established value. The new values hint
at an abundance of volatile elements (i.e. C, N, O, Ne) close to previous
results of Grevesse \& Sauval 1998, whereas the abundance of refractory
elements (i.e. Mg, Si, S, Fe) is considerably increased. Using the Linear Solar
Model formalism, we determine the variation of helioseismological observables
in response to the changes in elemental abundances, in order to explore the
consistency of these new measurements with constraints from helioseismology. We
find that, for observables that are particularly sensitive to the abundance of
volatile elements, in particular the radius of the convective zone boundary
(CZB) and the sound speed around the radius of CZB, improved agreement over
previous models is obtained. Conversely, the high abundance of refractories
correlates with a higher core temperature, resulting in an overproduction of
neutrinos and a huge increase in the surface Helium abundance. We conclude that
the "solar modelling problem" remains unsolved.
