Beryllium and the formation of the Thick Disk and of the Halo

Details Beryllium and the formation of the Thick Disk and of the Halo Beryllium and the formation of the Thick Disk and of the Halo

Mar 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009iaus..254..203p&link_type=abstract

The Galaxy Disk in Cosmological Context, Proceedings of the International Astronomical Union, IAU Symposium, Volume 254. Edited

Mathematics

Logic

Stars: Abundances, Galaxy: Halo, Galaxy: Disk

Scientific paper

We use Beryllium to investigate star formation in the early Galaxy. Be has been demonstrated to be a good indicator of time in these early epochs. By analyzing the so-far largest sample of halo and thick disk metal poor stars, we find a clear scatter in Be for a given value of [Fe/H] and [O/H]. The scatter is very pronounced for Halo stars, while it is marginal for thick disk stars. Our halo stars separate in the [α/Fe] - Be diagram, showing two main branches: one indistinguishable from the thick disk stars, and one with lower [α/Fe] ratio. The stars belonging to this branch are characterized by highly eccentric orbits and small perigalactic radius (Rmin). Their kinematics are consistent with an accreted component.

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