Volume 436, Number 3, June IV 2005
|Page(s)||L57 - L60|
|Published online||03 June 2005|
Letter to the Editor
Early star formation in the Galaxy from beryllium and oxygen abundances
European Southern Observatory, Garching bei München, Germany e-mail: email@example.com
2 INAF – Osservatorio di Arcetri, Firenze, Italy
3 INAF – Osservatorio di Padova, Padova, Italy
4 INAF – Osservatorio di Trieste, Trieste, Italy
5 Dipartimento di Fisica, Università di Pisa, Italy
Accepted: 10 May 2005
We investigate the evolution of the star formation rate in the early Galaxy using beryllium and oxygen abundances in metal poor stars. Specifically, we show that stars belonging to two previously identified kinematical classes (the so-called “accretion” and “dissipative” populations) are neatly separated in the [O/Fe] vs. diagram. The dissipative population follows the predictions of our model of Galactic evolution for the thick disk component, suggesting that the formation of this stellar population occurred on a timescale significantly longer (by a factor ∼5–10) than the accretion component. The latter shows a large scatter in the [O/Fe] vs. diagram, probably resulting from the inhomogeneous enrichment in oxygen and iron of the protogalactic gas. Despite the limitation of the sample, the data suggest that the combined use of products of spallation reactions (like beryllium) and elemental ratios of stellar nucleosynthesis products (like [O/Fe]) can constrain theoretical models for the formation and early evolution of our Galaxy.
Key words: stars: abundances / stars: age, late-type / Galaxy: halo / Galaxy: thick disk
© ESO, 2005
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.