2006/10/04 by M. Aldenius, Joel D. Tanner, J. D. Tanner +5 · 1 citation
Physics and Astronomy · #Abundance (ecology) #Astronomical spectroscopy #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atomic and Molecular Physics #Context (archaeology) #Galaxy #Observable #Optics #Oscillator strength #Physics #Quantum mechanics #Radiative transfer #Spectral line #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20066266
published as Astron.Astrophys. 461 (2007) 767-773 · Accepted for publication in A&A, 8 pages, 6 figures, Eq. 7 corrected
openalex publication_date 2006/10/04 · arxiv created 2006/10/06 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context.The stellar abundance ratio of Mg/Fe is an important tool in diagnostics of galaxy evolution. In order to make reliable measurements of the Mg abundance of stars, it is necessary to have accurate values for the oscillator strength (f-value) of each of the observable transitions. In metal-poor stars the 3p–4s triplet around 5175 Å (Fraunhofer's so-called b lines) are the most prominent magnesium lines. The lines also appear as strong features in the solar spectrum.