Helioseismic determination of the Solar metal mass fraction

The solar chemical composition is a key element entering both solar en stellar models. Due to the role of the Sun as reference in the metallicity scale used to determine the metallicity of distant stars. Therefore, knowing the chemical composition of the Sun is not only relevant for solar modelling but also for the choice of physical elements entering the stellar model grids. Following the revision in the early 2000s of the solar heavy element content (Asplund et al. 2004), an ongoing debate has agitated the solar modelling community as keeping a high solar metallicity (as in the Grevesse & Sauval 1998 tables) would provide a much better agreement with classical helioseismic constraints (sound speed, base of the convective envelope position, ...). The recent picture regarding spectroscopic determinations of solar abundances provided by Asplund et al. 2021 has been recently challenged in a paper by Magg et al. 2022, revising the solar metallicity back to its value of 1998. Independently of the controversy in spectroscopy, helioseismic determinations of the solar metallicity have been attempted in various papers (Lin & Däppen, Antia & Basu, Lin,Antia & Basu, Vorontsov et al. 2013, Buldgen et al. 2017). The latest studies favoured a low metallicity value, but suffered from very low precision. In this poster, we present an improved determination of the solar metallicity from helioseismic inversions and show that for all modern equations of state, we find a precise solar metallicity value in agreement with the Asplund et al. (2021) abundances, rejecting the Magg et al. (2022) values