March 5, 2009 Journal article Closed Access

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

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  <identifier identifierType="URL">https://www.openaccessrepository.it/record/180404</identifier>
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    <creator>
      <creatorName>Pasquini, Luca</creatorName>
      <givenName>Luca</givenName>
      <familyName>Pasquini</familyName>
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    <creator>
      <creatorName>Smiljanic, R.</creatorName>
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      <creatorName>Bonifacio, P.</creatorName>
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      <creatorName>Gratton, R.</creatorName>
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      <creatorName>Galli, D.</creatorName>
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      <creatorName>Randich, S.</creatorName>
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      <familyName>Randich</familyName>
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  <titles>
    <title>Beryllium and the formation of the Thick Disk and of the Halo</title>
  </titles>
  <publisher>INFN Open Access Repository</publisher>
  <publicationYear>2009</publicationYear>
  <subjects>
    <subject>Astronomy and Astrophysics</subject>
    <subject>Space and Planetary Science</subject>
  </subjects>
  <dates>
    <date dateType="Issued">2009-03-05</date>
  </dates>
  <language>en</language>
  <resourceType resourceTypeGeneral="Text">Journal article</resourceType>
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    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsIdenticalTo">10.1017/s1743921308027609</relatedIdentifier>
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    <rights rightsURI="info:eu-repo/semantics/closedAccess">Closed Access</rights>
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  <descriptions>
    <description descriptionType="Abstract">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.</description>
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