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We critically examine recent claims of a high solar metallicity by vonSteiger \& Zurbuchen (2016) based on \textit{in situ} measurements of the solarwind, rather than the standard spectroscopically-inferred abundances (Asplundet al. 2009). We test the claim by Vagnozzi et al. (2016) that a compositionbased on the solar wind enables one to construct a standard solar model inagreement with helioseismological observations and thus solve the decades-oldsolar modelling problem. We show that, although some helioseismologicalobservables are improved compared to models computed with spectroscopicabundances, most are in fact worse. The high abundance of refractory elementsleads to an overproduction of neutrinos, with a predicted $^8$B flux that isnearly twice its observed value, and $^7$Be and CNO fluxes that areexperimentally ruled out at high confidence. A combined likelihood analysisshows that models using the vSZ16 abundances fare worse than AGSS09 despite ahigher metallicity. We also present astrophysical and spectroscopic argumentsshowing the vSZ16 composition to be an implausible representation of the solarinterior, identifying the first ionisation potential effect in the outer solaratmosphere and wind as the likely culprit.

Implications of solar wind measurements for solar models and composition