TY - JOUR
T1 - Creating and using large grids of precalculated model atmospheres for a rapid analysis of stellar spectra
AU - Zsargó, J.
AU - Fierro-Santillán, C. R.
AU - Klapp, J.
AU - Arrieta, A.
AU - Arias, L.
AU - Valencia, J. M.
AU - Sigalotti, L. Di G.
AU - Hareter, M.
AU - Puebla, R. E.
N1 - Publisher Copyright:
© ESO 2020.
PY - 2020/11/1
Y1 - 2020/11/1
N2 - 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 Teff the luminosity L, the metallicity Z, and three stellar wind parameters: the exponent β, the terminal velocity V∞, and the volume filling factor F. 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 with steps of 10 km s. 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.
AB - 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 Teff the luminosity L, the metallicity Z, and three stellar wind parameters: the exponent β, the terminal velocity V∞, and the volume filling factor F. 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 with steps of 10 km s. 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.
KW - Methods: data analysis
KW - Miscellaneous
KW - Stars: atmospheres
KW - Métodos
KW - análisis de datos
KW - varios
KW - Estrellas
KW - atmósferas
UR - http://www.scopus.com/inward/record.url?scp=85096031473&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202038066
DO - 10.1051/0004-6361/202038066
M3 - Artículo
AN - SCOPUS:85096031473
SN - 0004-6361
VL - 643
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A88
ER -