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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

Chemical evolution of the bulge of M31: predictions about abundance ratios

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Autor(es):
Marcon-Uchida, M. M. [1] ; Matteucci, F. [2, 3, 4] ; Lanfranchi, G. A. [1] ; Spitoni, E. [2] ; Grieco, V. [2]
Número total de Autores: 5
Afiliação do(s) autor(es):
[1] Univ Cruzeiro Sul, Nucleo Astrofis Teor, BR-01506000 Sao Paulo - Brazil
[2] Univ Trieste, Dipartimento Fis, Sez Astron, I-34131 Trieste - Italy
[3] INAF Trieste, I-34131 Trieste - Italy
[4] INFN Trieste, I-34134 Trieste - Italy
Número total de Afiliações: 4
Tipo de documento: Artigo Científico
Fonte: Monthly Notices of the Royal Astronomical Society; v. 447, n. 2, p. 1096-1102, FEB 21 2015.
Citações Web of Science: 0
Resumo

We aim to reproduce the chemical evolution of the bulge of M31 using a detailed chemical evolution model, including radial gas flows coming from the disc. We study the impact of the initial mass function, the star formation rate and the time-scale for bulge formation on the metallicity distribution function of stars. We compute several models of chemical evolution using the metallicity distribution of dwarf stars as an observational constraint for the bulge of M31. Then, using the model that best reproduces the metallicity distribution function, we predict the {[}X/Fe] versus {[}Fe/H] relations for several chemical elements (O, Mg, Si, Ca, C, N). Our best model for the bulge of M31 is obtained by using a robust statistical method and assumes a Salpeter initial mass function, a Schmidt-Kennicutt law for star formation with an exponent k = 1.5, an efficiency of star formation of similar to 15 +/- 0.27 Gyr(-1) and an infall time-scale of similar to 0.10 +/- 0.03 Gyr. Our results suggest that the bulge of M31 formed very quickly as a result of an intense star formation rate and an initial mass function flatter than in the solar vicinity but similar to that inferred for the Milky Way bulge. The {[}alpha/Fe] ratios in the stars of the bulge of M31 should be high for most of the {[}Fe/H] range, as observed in the Milky Way bulge. These predictions await future data to be proven. (AU)

Processo FAPESP: 10/17142-4 - Evolução química de galáxias próximas
Beneficiário:Monica Midori Marcon Uchida Sguazzardi
Linha de fomento: Bolsas no Brasil - Pós-Doutorado