2006/11/07 by L. Piersanti, O. Straniero, S. Cristallo · 1 citation
Physics and Astronomy · #Abundance (ecology) #Abundance of the chemical elements #Astro and Planetary Science #Astronomy and Astrophysical Research #Chemical composition #Formation and evolution of the Solar System #Photosphere #Solar System #Solar physics #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20054505
22 pages, 8 figures, accepted by A&A
arxiv created 2006/11/07 · openalex publication_date 2006/11/21 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context.The knowledge of isotopic and elemental abundances of the pristine solar system material provides a fundamental test of galactic chemical evolution models, while the composition of the solar photosphere is a reference pattern to understand stellar abundances. However, spectroscopic or meteoritic abundance determinations are only possible for an incomplete sample of the 83 elements detected in the solar system. Therefore, only relative abundances are experimentally determined, with respect to or to for spectroscopic or meteoritic measurements, respectively. For this reason, the available compilations of solar abundances are obtained by combining spectroscopic and meteoritic determinations, a procedure requiring the knowledge of the chemical modification occurring in the solar photosphere.