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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 (in)homogeneity and atomic diffusion in the open cluster M67

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Liu, F. [1] ; Asplund, M. [2, 3] ; Yong, D. [2, 3] ; Feltzing, S. [1] ; Dotter, A. [4] ; Melendez, J. [5] ; Ramirez, I. [6]
Número total de Autores: 7
Afiliação do(s) autor(es):
[1] Lund Univ, Dept Astron & Theoret Phys, Lund Observ, Box 43, S-22100 Lund - Sweden
[2] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611 - Australia
[3] ARC Ctr Excellence All Sky Astrophys 3 Dimens AST, Canberra, ACT - Australia
[4] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 - USA
[5] Univ Sao Paulo, IAG, Dept Astron, Rua Matao 1226, BR-05508900 Sao Paulo, SP - Brazil
[6] Tacoma Community Coll, Tacoma, WA - USA
Número total de Afiliações: 6
Tipo de documento: Artigo Científico
Fonte: Astronomy & Astrophysics; v. 627, JUL 10 2019.
Citações Web of Science: 3

Context. The benchmark open cluster M67 is known to have solar metallicity and an age similar to that of the Sun. It thus provides us with a great opportunity to study the properties of solar twins, as well as the evolution of Sun-like stars. Aims. Previous spectroscopic studies of M67 reported possible subtle changes in stellar surface abundances throughout the stellar evolutionary phase, namely the effect of atomic diffusion. In this study we attempt to confirm and quantify more precisely the effect of atomic diffusion, and to explore the level of chemical (in)homogeneity in M67. Methods. We presented a strictly line-by-line differential chemical abundance analysis of two groups of stars in M67: three turn-off stars and three subgiants. Stellar atmospheric parameters and elemental abundances were obtained with very high precision using the Keck/HIRES spectra. Results. The subgiants in our sample show negligible abundance variations (<= 0.02 dex), which implies that M67 was born chemically homogeneous. We note that there is a significant abundance difference (similar to 0.1-0.2 dex) between subgiants and turn-off stars, which can be interpreted as the signature of atomic diffusion. Qualitatively stellar models with diffusion agree with the observed abundance results. Some turn-off stars do not follow the general pattern, which suggests that in some cases diffusion can be inhibited, or they might have undergone some sort of mixing event related to planets. Conclusions. Our results pose additional challenges for chemical tagging when using turn-off stars. In particular, the effects of atomic diffusion, which could be as large as 0.1-0.2 dex, must be taken into account in order for chemical tagging to be successfully applied. (AU)

Processo FAPESP: 18/04055-8 - Espectroscopia de alta precisão: das primeiras estrelas aos planetas
Beneficiário:Jorge Luis Melendez Moreno
Linha de fomento: Auxílio à Pesquisa - Temático