The chemical composition of the Sun is primarily determined from the analysis of the solar photospheric spectrum. Comparisons between solar and meteoritic abundances show a good agreement, leading to the construction of the Standard Abundance Distribution (SAD). Key words include Sun: abundances, Meteorites: abundances, Solar spectroscopy. Abbreviations include CI – Carbonaceous Chondrite; SW – Solar Wind; SEP – Solar Energetic Particles; SAD – Standard Abundance Distribution. Historically, H.N. Russell conducted the first quantitative analysis of the solar atmosphere in 1929, determining the abundances of 56 elements. His results were widely used and showed that the solar atmosphere and universe are mainly composed of hydrogen. Twenty years later, Unsöld improved upon Russell's work, finding similar results and praising his spectroscopic skills. Over the years, advancements in techniques and models have improved the accuracy of abundance analyses. The curve of growth technique, developed by Minnacert, and the photospheric model by Strömgren, contributed to more precise results. Goldberg et al. (1960) used these methods to determine abundances for 42 elements, which became a standard reference for over a decade. In recent years, various groups have contributed to photospheric abundance studies. Solar abundances are derived from multiple sources, including spectroscopy, particle collection techniques, and solar models. The Sun's chemical composition varies in different layers and over time, with element migration occurring below the convection zone. The solar outer layers show variations in composition, with a fractionation effect leading to the FIP or FIT effect. The solar photosphere provides the most data, with a large number of elements present in its spectrum. Other sources of solar abundances concern fewer elements. The workshop discussed various aspects of solar composition, including the effects of element migration and fractionation in different solar layers.The chemical composition of the Sun is primarily determined from the analysis of the solar photospheric spectrum. Comparisons between solar and meteoritic abundances show a good agreement, leading to the construction of the Standard Abundance Distribution (SAD). Key words include Sun: abundances, Meteorites: abundances, Solar spectroscopy. Abbreviations include CI – Carbonaceous Chondrite; SW – Solar Wind; SEP – Solar Energetic Particles; SAD – Standard Abundance Distribution. Historically, H.N. Russell conducted the first quantitative analysis of the solar atmosphere in 1929, determining the abundances of 56 elements. His results were widely used and showed that the solar atmosphere and universe are mainly composed of hydrogen. Twenty years later, Unsöld improved upon Russell's work, finding similar results and praising his spectroscopic skills. Over the years, advancements in techniques and models have improved the accuracy of abundance analyses. The curve of growth technique, developed by Minnacert, and the photospheric model by Strömgren, contributed to more precise results. Goldberg et al. (1960) used these methods to determine abundances for 42 elements, which became a standard reference for over a decade. In recent years, various groups have contributed to photospheric abundance studies. Solar abundances are derived from multiple sources, including spectroscopy, particle collection techniques, and solar models. The Sun's chemical composition varies in different layers and over time, with element migration occurring below the convection zone. The solar outer layers show variations in composition, with a fractionation effect leading to the FIP or FIT effect. The solar photosphere provides the most data, with a large number of elements present in its spectrum. Other sources of solar abundances concern fewer elements. The workshop discussed various aspects of solar composition, including the effects of element migration and fractionation in different solar layers.