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Chemodynamical evolution of the Milky Way disk: I. The solar vicinity

Minchev, I ; Chiappini, C ; Martig, M

Astronomy and astrophysics (Berlin), 2013-10, Vol.558, p.np-np [Periódico revisado por pares]

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Título:
Chemodynamical evolution of the Milky Way disk: I. The solar vicinity
Autor: Minchev, I ; Chiappini, C ; Martig, M
Assuntos: Astronomical models ; Chemical evolution ; Computer simulation ; Disks ; Enrichment ; Evolution ; Mathematical models ; Milky Way Galaxy
É parte de: Astronomy and astrophysics (Berlin), 2013-10, Vol.558, p.np-np
Notas: ObjectType-Article-1
SourceType-Scholarly Journals-1
ObjectType-Feature-2
content type line 23
Descrição: In the first paper of this series, we present a new approach for studying the chemo-dynamical evolution in disk galaxies, which consist of fusing disk chemical evolution models with compatible numerical simulations of galactic disks. This method avoids known star formation and chemical enrichment problems encountered in simulations. Here we focus on the Milky Way, by using a detailed thin-disk chemical evolution model and a simulation in the cosmological context, with dynamical properties close to those of our Galaxy. We show that in the absence of early-on massive mergers the vertical velocity dispersion of the oldest stars is underestimated by a factor of ~2 compared with observations. We can, therefore, argue that the Milky Way thick disk is unlikely to have been formed through a quiescent disk evolution. An observational test involving both chemical and kinematic information must be devised to ascertain this possibility.
Idioma: Inglês

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