The solar chemical composition is crucial for understanding the formation, structure, and evolution of the Sun and our solar system. This review evaluates the current understanding of the solar photospheric composition, presenting a re-determination of the abundances of nearly all available elements using a realistic 3-dimensional (3D) time-dependent hydrodynamical model of the solar atmosphere. The new abundances show significantly lower values for carbon, nitrogen, oxygen, and neon compared to previously used values. The results are supported by internal consistency and agreement with values from the solar neighborhood and pristine meteorites, but conflict with standard models of the solar interior based on helioseismology. The review discusses the methodology, including observations, atomic and molecular data, solar atmospheric and line formation modeling, and observational constraints. It also compares the new abundances with those inferred from meteorites, the solar neighborhood, helioseismology, and solar neutrinos. The final section summarizes key points and outlines future issues.The solar chemical composition is crucial for understanding the formation, structure, and evolution of the Sun and our solar system. This review evaluates the current understanding of the solar photospheric composition, presenting a re-determination of the abundances of nearly all available elements using a realistic 3-dimensional (3D) time-dependent hydrodynamical model of the solar atmosphere. The new abundances show significantly lower values for carbon, nitrogen, oxygen, and neon compared to previously used values. The results are supported by internal consistency and agreement with values from the solar neighborhood and pristine meteorites, but conflict with standard models of the solar interior based on helioseismology. The review discusses the methodology, including observations, atomic and molecular data, solar atmospheric and line formation modeling, and observational constraints. It also compares the new abundances with those inferred from meteorites, the solar neighborhood, helioseismology, and solar neutrinos. The final section summarizes key points and outlines future issues.