TY - GEN
T1 - Creating and Using Large Grids of Pre-calculated Model Atmospheres for Rapid Analysis of Stellar Spectra
AU - Zsargó, Janos
AU - Fierro-Santillán, Celia Rosa
AU - Klapp, Jaime
AU - Arrieta, Anabel
AU - Arias, Lorena
AU - Valencia, Jurij Mendoza
AU - Di G. Sigalotti, Leonardo
N1 - Publisher Copyright:
© Springer Nature Switzerland AG 2019.
PY - 2019
Y1 - 2019
N2 - We present a database of 45,000 atmospheric models (which will become 80,000 models by the end of the project) with stellar masses between 9 and 120M(Formula Presented), covering the region of the OB main sequence and W-R stars in the H–R diagram. The models were calculated using the ABACUS I supercomputer and the stellar atmosphere code CMFGEN. The parameter space has 6 dimensions: the effective temperature Teff, the luminosity L, the metallicity Z, and three stellar wind parameters, namely the exponent β, the terminal velocity V∞, and the volume filling factor Fcl. For each model, we also calculate synthetic spectra in the UV (900–2000 Å), optical (3500–7000 Å), and near IR (10000–30000 Å) regions. To facilitate comparison with observations, the synthetic spectra were rotationally broaden using ROTIN3, by covering v sin i velocities between 10 and 350 km/s−1 with steps of 10 km/s−1, resulting in a library of 1 575 000 synthetic spectra. In order to demonstrate the benefits of employing the databases of pre-calculated models, we also present the results of the re-analysis of ε Ori by using our grid.
AB - We present a database of 45,000 atmospheric models (which will become 80,000 models by the end of the project) with stellar masses between 9 and 120M(Formula Presented), covering the region of the OB main sequence and W-R stars in the H–R diagram. The models were calculated using the ABACUS I supercomputer and the stellar atmosphere code CMFGEN. The parameter space has 6 dimensions: the effective temperature Teff, the luminosity L, the metallicity Z, and three stellar wind parameters, namely the exponent β, the terminal velocity V∞, and the volume filling factor Fcl. For each model, we also calculate synthetic spectra in the UV (900–2000 Å), optical (3500–7000 Å), and near IR (10000–30000 Å) regions. To facilitate comparison with observations, the synthetic spectra were rotationally broaden using ROTIN3, by covering v sin i velocities between 10 and 350 km/s−1 with steps of 10 km/s−1, resulting in a library of 1 575 000 synthetic spectra. In order to demonstrate the benefits of employing the databases of pre-calculated models, we also present the results of the re-analysis of ε Ori by using our grid.
KW - Astronomical databases: miscellaneous
KW - Methods: data analysis
KW - Stars: atmospheres
UR - http://www.scopus.com/inward/record.url?scp=85077497515&partnerID=8YFLogxK
U2 - 10.1007/978-3-030-38043-4_19
DO - 10.1007/978-3-030-38043-4_19
M3 - Contribución a la conferencia
AN - SCOPUS:85077497515
SN - 9783030380427
T3 - Communications in Computer and Information Science
SP - 227
EP - 236
BT - Supercomputing - 10th International Conference on Supercomputing in Mexico, ISUM 2019, Revised Selected Papers
A2 - Torres, Moisés
A2 - Klapp, Jaime
PB - Springer
T2 - 10th International Conference on Supercomputing, ISUM 2019
Y2 - 25 March 2019 through 29 March 2019
ER -