A dynamical evolution study of the open clusters: Berkeley 10, Berkeley 81, Berkeley 89 and Ruprecht 135

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cakmak H., Karatas Y.

NEW ASTRONOMY, cilt.96, 2022 (SCI-Expanded) identifier identifier identifier

  • Yayın Türü: Makale / Tam Makale
  • Cilt numarası: 96
  • Basım Tarihi: 2022
  • Doi Numarası: 10.1016/j.newast.2022.101833
  • Dergi Adı: NEW ASTRONOMY
  • Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Academic Search Premier, Aerospace Database, Communication Abstracts, INSPEC, Metadex, Civil Engineering Abstracts
  • Anahtar Kelimeler: <p>(Galaxy:) open clusters and associations:general</p>, <p>(Galaxy:) open clusters and associations:individual</p>, Galaxy: stellar content, GALACTIC OPEN CLUSTERS, STAR-CLUSTERS, THEORETICAL ISOCHRONES, SPIRAL STRUCTURE, PROPER MOTIONS, NGC 1817, PHOTOMETRY, SYSTEMS, SIMULATIONS, MEMBERSHIP
  • İstanbul Üniversitesi Adresli: Evet

Özet

By utilizing Gaia EDR3 photometric/astrometric data, we studied the dynamical evolution from the obtained astrophysical, structural and dynamical parameters of the open clusters (OCs), Berkeley 10 (Be 10), Berkeley 81 (Be 81), Berkeley 89 (Be 89), and Ruprecht 135 (Ru 135). The Gaia EDR3 photometric distances from the isochrone fitting method are smaller than the ones of Gaia EDR2. The relaxation times of four OCs are smaller than their ages, in this regard, they are dynamically relaxed. Their steep overall mass function slopes mean that their low mass stars outnumber their massive ones. Their large tau/relatively small t(r/x & nbsp;)values imply an advanced mass segregation. Therefore, they seem to have lost their low-mass stars much to the field. Be 89's outer parts indicate an expansion with time. However, Be 10 and Be 81 show the relatively shrinkage core/cluster radii due to dynamical evolution. Ru 135 (1.0 Gyr) may have a primordial origin, instead of shrinking in size and mass with time. Be 89's tidal radius is less than its cluster radius. This means that its member stars lie within its tidal radius, in the sense it is gravitationally bound to the cluster. For the rest OCs, the cluster members beyond their tidal radii are gravitationally unbound to the clusters, which are more influenced by the potential of the Galaxy.