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arXiv:astro-ph/0004157 (astro-ph)
[Submitted on 12 Apr 2000]

Title:Abundances of light elements in metal-poor stars. IV. [Fe/O] and [Fe/Mg] and the history of star formation in the solar neighborhood

Authors:Raffaele Gratton (1), Eugenio Carretta (1), Francesca Matteucci (2), Chris Sneden (3) ((1) Osservatorio Astronomico di Padova, ITALY, (2) SISSA, Trieste, ITALY, (3) University of Texas at Austin and McDonald Observatory, USA)
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Abstract: The accurate O, Mg and Fe abundances derived in previous papers of this series from a homogenous reanalysis of high quality data for a large sample of stars are combined with stellar kinematics in order to discuss the history of star formation in the solar neighborhood. We found that the Fe/O and Fe/Mg abundance ratios are roughly constant in the (inner) halo and the thick disk; this means that the timescale of halo collapse was shorter than or of the same order of typical lifetime of progenitors of type Ia SNe (~ 1 Gyr), this conclusion being somewhat relaxed (referring to star formation in the individual fragments) in an accretion model for the Galaxy formation. Both Fe/O and Fe/Mg ratios raised by ~ 0.2 dex while the O/H and Mg/H ratios hold constant during the transition from the thick to thin disk phases, indicating a sudden decrease in star formation in the solar neighbourhood at that epoch. These results are discussed in the framework of current views of Galaxy formation; they fit in a scenario where both dissipational collapse and accretions were active on a quite similar timescale.
Comments: 13 pages, 9 encapsulated figures. LaTeX, uses this http URL. Accepted for publication in Astronomy & Astrophysics
Subjects: Astrophysics (astro-ph)
Cite as: arXiv:astro-ph/0004157
  (or arXiv:astro-ph/0004157v1 for this version)
  https://doi.org/10.48550/arXiv.astro-ph/0004157

Submission history

From: Eugenio Carretta [view email]
[v1] Wed, 12 Apr 2000 12:31:08 UTC (80 KB)
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