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CHEMICALSUBSTRUCTURE

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Elemental abundance analysis of substructures in the Galaxy disk. Implications f...

Elemental abundance analysis of substructures in the Galaxy disk. Implications for disk formation Elemental abundances in stars have proved to be an important tool in the study of the formation and evolution of the Milky Way. Combining the elemental abundances with the motions of the stars provide even stronger evidence for pa... ver más

24/11/2011

174K€

Presupuesto del proyecto: 174K€

Líder del proyecto

MAX IV Laboratory, Lund University No se ha especificado una descripción o un objeto social para esta compañía.

Fecha límite participación Sin fecha límite de participación.

Financiación concedida El organismo FP7 notifico la concesión del proyecto el día 2011-11-24 No tenemos la información de la convocatoria

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1 Participantes

173.89K€ | Lider

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Líder del proyecto

MAX IV Laboratory, Lund University No se ha especificado una descripción o un objeto social para esta compañía.

Presupuesto del proyecto 174K€

Fecha límite de participación Sin fecha límite de participación.

Descripción del proyecto Elemental abundances in stars have proved to be an important tool in the study of the formation and evolution of the Milky Way. Combining the elemental abundances with the motions of the stars provide even stronger evidence for past and present evolution. Much recent work has focused on the identification of stellar streams in the Milky Way halo. Some of these streams have been identified as ruptured dwarf galaxies that are currently being engulfed by our Galaxy. However, it is the thin disk that dynamically and morphologically is the defining part of a disk galaxy. Several studies utilizing the Hipparcos data have unveiled a multitude of substructure within the thin disk. The origin of these substructures is not clear. Stars form in clusters and depending on their mass they may lose all or some of the cluster stars to the general field. As the cluster orbits around the Galaxy, it will disperse into a tube-like structure around the galactic plane. After several orbits it dissolves into the general background. The stars from the original cluster will be spread over the sky, but can be identified as a group through their common space motion. Hence, dissolving cluster can be one explanation for the substructures. Dynamical evolution within the disk and interaction with the bar can be another explanation. By obtaining elemental abundances of dispersing clusters and their associated superclusters and/or moving groups we can find out if they all come from the same original cluster (i.e. they have the same elemental abundance pattern) or if the structure is simply due to stirring of the general disk population (the stars do not share the same abundance pattern). We propose a comprehensive study of open clusters and associated groups as well as a truly differential study between these substructures and the Milky Way field population in order to shed light on how much of the disk population comes from dispersing clusters and how common the dynamical substructures are.

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