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

Simple item page
dc.creatorGratton, Raffaele
dc.creatorCarretta, Eugenio
dc.creatorMatteucci, Francesca
dc.creatorSneden, Chris
dc.date2000-04-12
dc.date.accessioned2026-07-07T01:53:07Z
dc.date.available2026-07-07T01:53:07Z
dc.descriptionThe 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.
dc.description13 pages, 9 encapsulated figures. LaTeX, uses l-aa.sty. Accepted for publication in Astronomy & Astrophysics
dc.identifierhttps://arxiv.org/abs/astro-ph/0004157
dc.identifierhttp://arxiv.org/abs/astro-ph/0004157
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/850
dc.subjectAstrophysics
dc.titleAbundances of light elements in metal-poor stars. IV. [Fe/O] and [Fe/Mg] and the history of star formation in the solar neighborhood
dc.typetext

Files

Collections

arXiv