The solar chemical composition is a key reference in astronomy, used to compare the elemental content of cosmic objects. Recent studies using 3D hydrodynamical models of the solar atmosphere have significantly revised solar abundances, reducing the metal content in the solar convection zone by almost a factor of two compared to previous compilations. These revisions challenge traditional models and raise questions for helioseismology. The solar abundance analysis, based on a 3D model, shows improved agreement with various atomic and molecular indicators, particularly for elements like carbon, nitrogen, and oxygen. The new abundances are slightly lower than previously recommended values, with differences typically around 0.05–0.10 dex. The revised solar abundances now align better with local interstellar medium and nearby B star measurements. However, they introduce new challenges for helioseismology, as the revised abundances for C, N, O, and Ne significantly alter the solar interior structure, leading to worse agreement with observed sound speeds. The new abundances also remove the Sun's special status compared to its neighborhood. Despite these challenges, the 3D models provide more realistic results, and the agreement between observed and predicted line profiles is excellent. Continued improvements in atomic and molecular data are essential for accurate abundance determinations. The study highlights the importance of refining solar abundance data and the need for further research to resolve discrepancies between solar and meteoritic abundances.The solar chemical composition is a key reference in astronomy, used to compare the elemental content of cosmic objects. Recent studies using 3D hydrodynamical models of the solar atmosphere have significantly revised solar abundances, reducing the metal content in the solar convection zone by almost a factor of two compared to previous compilations. These revisions challenge traditional models and raise questions for helioseismology. The solar abundance analysis, based on a 3D model, shows improved agreement with various atomic and molecular indicators, particularly for elements like carbon, nitrogen, and oxygen. The new abundances are slightly lower than previously recommended values, with differences typically around 0.05–0.10 dex. The revised solar abundances now align better with local interstellar medium and nearby B star measurements. However, they introduce new challenges for helioseismology, as the revised abundances for C, N, O, and Ne significantly alter the solar interior structure, leading to worse agreement with observed sound speeds. The new abundances also remove the Sun's special status compared to its neighborhood. Despite these challenges, the 3D models provide more realistic results, and the agreement between observed and predicted line profiles is excellent. Continued improvements in atomic and molecular data are essential for accurate abundance determinations. The study highlights the importance of refining solar abundance data and the need for further research to resolve discrepancies between solar and meteoritic abundances.