The solar metallicity issue is a long-lasting problem of astrophysics , impacting multiple fields and still subject to debate and uncertainties .
While spectroscopy has mostly been used to determine the solar heavy elements abundance , helioseismologists attempted providing a seismic determination of the metallicity in the solar convective enveloppe .
However , the puzzle remains since two independent groups prodived two radically different values for this crucial astrophysical parameter .
We aim at providing an independent seismic measurement of the solar metallicity in the convective enveloppe .
Our main goal is to help provide new information to break the current stalemate amongst seismic determinations of the solar heavy element abundance .
We start by presenting the kernels , the inversion technique and the target function of the inversion we have developed .
We then test our approach in multiple hare-and-hounds exercises to assess its reliability and accuracy .
We then apply our technique to solar data using calibrated solar models and determine an interval of seismic measurements for the solar metallicity .
We show that our inversion can indeed be used to estimate the solar metallicity thanks to our hare-and-hounds exercises .
However , we also show that further dependencies in the physical ingredients of solar models lead to a low accuracy .
Nevertheless , using various physical ingredients for our solar models , we determine metallicity values between 0.008 and 0.014 .