2020/09/10 by J. Zsargó, J. Zsargo, C. Fierro +11 · 8 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Atmosphere (unit) #Computational physics #Effective temperature #Galaxy #Geometry #Luminosity #Materials science #Metallicity #Meteorology #Parameter space #Physics #Range (aeronautics) #Spectral line #Stars #Stellar atmosphere #Stellar, planetary, and galactic studies #astro-ph.IM #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/202038066
published in Astronomy and Astrophysics 643, A88 (EDP Sciences) · 22 pages, 18 figures, accepted for publication in A&A
openalex publication_date 2020/09/10 · arxiv created 2020/09/23 · arxiv updated 2020/11/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Aims. We present a database of 43 340 atmospheric models (∼80 000 models at the conclusion of the project) for stars with stellar masses between 9 and 120 M ⊙ , covering the region of the OB main-sequence and Wolf-Rayet stars in the Hertzsprung-Russell diagram. Methods. The models were calculated using the ABACUS I supercomputer and the stellar atmosphere code CMFGEN. Results. The parameter space has six dimensions: the effective temperature T eff , the luminosity L , the metallicity Z , and three stellar wind parameters: the exponent β , the terminal velocity V ∞ , and the volume filling factor F cl . For each model, we also calculate synthetic spectra in the UV (900−2000 Å), optical (3500−7000 Å), and near-IR (10 000−40 000 Å) regions. To facilitate comparison with observations, the synthetic spectra can be rotationally broadened using ROTIN3, by covering v sin i velocities between 10 and 350 km s −1 with steps of 10 km s −1 . Conclusions. We also present the results of the reanalysis of ϵ Ori using our grid to demonstrate the benefits of databases of precalculated models. Our analysis succeeded in reproducing the best-fit parameter ranges of the original study, although our results favor the higher end of the mass-loss range and a lower level of clumping. Our results indirectly suggest that the resonance lines in the UV range are strongly affected by the velocity-space porosity, as has been suggested by recent theoretical calculations and numerical simulations.