  In the past years, a systematic downward revision of the metallicity of the
Sun has led to the "solar modeling problem", namely the disagreement between
predictions of standard solar models and inferences from helioseismology.
Recent solar wind measurements of the metallicity of the Sun, however, provide
once more an indication of a high-metallicity Sun. Because of the effects of
possible residual fractionation, the derived value of the metallicity
$Z_{\odot} = 0.0196 \pm 0.0014$ actually represents a lower limit to the true
metallicity of the Sun. However, when compared with helioseismological
measurements, solar models computed using these new abundances fail to restore
agreement, owing to the implausibly high abundance of refractory (Mg, Si, S,
Fe) elements, which correlates with a higher core temperature and hence an
overproduction of solar neutrinos. Moreover, the robustness of these
measurements is challenged by possible first ionization potential fractionation
processes. I will discuss these solar wind measurements, which leave the "solar
modeling problem" unsolved.
