Potential contributions of Pop III and intermediate-mass Pop II stars to cosmic chemical enrichment

Autor(es)

Corazza, Lia C. C. ; Miranda, Oswaldo D. D. ; Wuensche, Carlos A. A.

• Tipo de documento: Artigo Científico
• Fonte: Astronomy & Astrophysics; v. 668, p. 14-pg., 2022-12-20.

Resumo

Context. We propose a semi-analytic model that is developed to understand the cosmological evolution of the mean metallicity in the Universe. In particular, we study the contributions of Population III (Pop III) and Population II (Pop II) stars to the production of Fe, Si, Zn, Ni, P, Mg, Al, S, C, N, and O. Aims. We aim to quantify the roles of two different models in the chemical enrichment of the Universe. The first model (A) considers both stars with Pop III and Pop II yields. For the second model (B), the yields involved are only for Pop II stars. Methods. We start by describing the cosmic star formation rate (CSFR) through an adaptation of a scenario developed within the hierarchical scenario of structure formation with a Press-Schechter-like formalism. We adapt the formalism to implement the CSFR to the standard chemical evolution scenario to investigate the course of chemical evolution on a cosmological basis. Calculations start at redshift z;similar to;20, and we compare the results of our two models with data from damped Lyman-alpha systems (DLAs), and globular clusters (GCs). Results. Our main results find that metal production in the Universe occurred very early, quickly increasing with the formation of the first stars. When comparing results for [Fe/H] with observations from GCs, yields of Pop II stars are not enough to explain the observed chemical abundances, requiring stars with physical properties similar those expected from Pop III stars. Conclusions. Our semi-analytic model can deliver consistent results for the evolution of cosmic metallicities. Our results show that the chemical enrichment in the early Universe is rapid, and at redshift similar to 12.5, the metallicity reaches 10(-4)Z(circle dot) for the model that includes Pop III stars. In addition, we explore values for the initial mass function (IMF) within the range [0.85, 1.85]. (AU)

• Processo FAPESP: 14/11156-4 - O que determina o crescimento da massa estelar de galáxias elípticas? Intrínseco ou ambiente: a saga contínua
• Beneficiário: Reinaldo Ramos de Carvalho
• Modalidade de apoio: Auxílio à Pesquisa - Temático