2009/11/27 by S. Simón-Díaz, S. Simón‐Díaz · 2 citations
Physics and Astronomy · #Abundance (ecology) #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Homogeneous #Main sequence #Nebula #Orion Nebula #Physics #Stars #Stellar atmosphere #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/200913120
18 tables, 10 figures, acepted to be published in A&A
openalex publication_date 2009/11/27 · arxiv created 2009/12/21 · arxiv updated 2015/05/14 · openalex created_date 2022/09/16 · openalex updated_date 2026/08/05
<i>Context. <i/>Recent accurate abundance analyses of B-type main sequence stars in the solar vicinity has shown that abundances derived from these stellar objects are more homogeneous and metal-rich than previously thought.<i>Aims. <i/>We investigate whether the inhomogeneity of abundances previously found in B-type stars in the Ori OB1 association is real (hence a signature of enrichment of the newly formed stars in an induced star formation scenario) or a consequence of intrinsic errors induced by the use of photometric indices to establish the stellar parameters prior to the abundance analysis.<i>Methods. <i/>We obtained a new (improved) spectroscopic data set comprising 13 B-type stars in the various Ori OB1 associations, and performed a detailed, self-consistent spectroscopic abundance analysis by means of the modern stellar atmosphere code fastwind.<i>Results. <i/>We detect systematic errors in the stellar parameters determined previously which affect the derived abundances. Once these errors are accounted for, we find a high degree of homogeneity in the O and Si abundances for stars in the four Ori OB1 subgroups. The derived abundances are in very good agreement with recent determinations in other B-type stars in the solar vicinity. We also compare our results with those obtained for the Sun during the epoch of the ”solar crisis”, and the Orion nebula.