March 5, 2009 Journal article Closed Access

Pasquini, Luca; Smiljanic, R.; Bonifacio, P.; Gratton, R.; Galli, D.; Randich, S.

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  <dc:creator>Pasquini, Luca</dc:creator>
  <dc:creator>Smiljanic, R.</dc:creator>
  <dc:creator>Bonifacio, P.</dc:creator>
  <dc:creator>Gratton, R.</dc:creator>
  <dc:creator>Galli, D.</dc:creator>
  <dc:creator>Randich, S.</dc:creator>
  <dc:date>2009-03-05</dc:date>
  <dc:description>AbstractWe 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.</dc:description>
  <dc:identifier>https://www.openaccessrepository.it/record/180404</dc:identifier>
  <dc:identifier>10.1017/s1743921308027609</dc:identifier>
  <dc:language>eng</dc:language>
  <dc:relation>url:https://www.openaccessrepository.it/communities/itmirror</dc:relation>
  <dc:rights>info:eu-repo/semantics/closedAccess</dc:rights>
  <dc:subject>Astronomy and Astrophysics</dc:subject>
  <dc:subject>Space and Planetary Science</dc:subject>
  <dc:title>Beryllium and the formation of the Thick Disk and of the Halo</dc:title>
  <dc:type>info:eu-repo/semantics/article</dc:type>
  <dc:type>publication-article</dc:type>
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