2002/10/31 by Thierry Lanz, T. Lanz, Ivan Hubeny +1 · 32 citations
Mathematics · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atomic and Molecular Physics #Galaxy #Geometry #Grid #Hydrostatic equilibrium #Limit (mathematics) #Line (geometry) #Mathematics #Physics #Redshift #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/374373
published as Astrophys.J.Suppl. 146 (2003) 417; Erratum-ibid. 147 (2003) 225 · 57 pages, 16 figures; minor additions and corrections; to appear in Astrophysical Journal Supplement, Vol. 146 (June 2003)
arxiv created 2003/02/14 · openalex publication_date 2003/06/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We have constructed a comprehensive grid of 680 metal line-blanketed, non-LTE, plane-parallel, hydrostatic model atmospheres for the basic parameters appropriate to O-type stars. The OSTAR2002 grid considers 12 values of effective temperatures, 27,500 K ≤ T eff ≤ 55,000 K with 2500 K steps, eight surface gravities, 3.0 ≤ log g ≤ 4.75 with 0.25 dex steps, and 10 chemical compositions, from metal-rich relative to the Sun to metal-free. The lower limit of log g for a given effective temperature is set by an approximate location of the Eddington limit. The selected chemical compositions have been chosen to cover a number of typical environments of massive stars: the Galactic center, the Magellanic Clouds, blue compact dwarf galaxies like I Zw 18, and galaxies at high redshifts. The paper contains a description of the OSTAR2002 grid and some illustrative examples and comparisons. The complete OSTAR2002 grid is available on-line.