Tag: Milky Way

Archeo-astronomy with the Gaia-ESO Survey. “The Gaia-ESO Survey: matching chemodynamical simulations to observations of the Milky Way” of B. B. Thompson recently published

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Not all the archaeologists do their studies digging holes or classifying artifacts in dusty museums… some of them actually use telescopes…   Galactic archeology is a branch of astronomy dedicated to the study of the formation and evolution of the components of our Galaxy (bulge, bar, disc and halo) by analyzing ages, dynamics, and chemical abundances of stars. Not an easy

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The chemical evolution of our Galaxy studied with GES. The study: “The Gaia-ESO Survey: Galactic evolution of sulphur and zinc” of S. Duffau published on A&A

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Stars more massive than 9 solar masses are efficient chemical labs, where hydrogen and helium are synthesized into other chemical elements, such as oxygen, carbon, and silicon. When these stars explode as supernovae (type I or “core-collpase” supernovae), these chemical elements are ejected into space, enriching the interstellar medium and being in future available to form new generations of stars.

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Published on A&A: “The Gaia-ESO Survey: radial distribution of abundances in the Galactic disc from open clusters and young-field stars” by L. Magrini

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Massive stars are enormous chemical laboratories where heavy chemical elements are synthesized. For instance, the alpha-elements (O, Mg, Si, Ca, and Ti) are produced by nucleosynthetic processes in the interior of massive stars. Moreover, the lifetime of massive stars is much shorter than that of low mass stars: few million years for the former compared to several billion of years

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Pubblicato su A&A “The Gaia-ESO Survey: the present-day radial metallicity distribution of the Galactic disc probed by pre-main-sequence clusters” di L. Spina

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di Mario Giuseppe Guarcello    ( segui mguarce)     Esistono vari modelli che cercano di spiegare la formazione e l’evoluzione del disco sottile della Via Lattea, della sua popolazione stellare e dei bracci a spirale. Uno dei parametri fondamentali per il processo di formazione stellare nel disco, la distribuzione di massa delle stelle, l’evoluzione stellare e la migrazione lungo il disco

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