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Verfasst von:Leveque, Agostino [VerfasserIn]   i
 Giersz, Mirek [VerfasserIn]   i
 Arca Sedda, Manuel [VerfasserIn]   i
 Askar, Abbas [VerfasserIn]   i
Titel:MOCCA-survey data base
Titelzusatz:extra galactic globular clusters - II. Milky Way and Andromeda
Verf.angabe:A. Leveque, M. Giersz, M. Arca-Sedda, Abbas Askar
E-Jahr:2022
Jahr:17 June 2022
Umfang:16 S.
Fussnoten:Gesehen am 15.09.2022
Titel Quelle:Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
Ort Quelle:Oxford : Oxford Univ. Press, 1827
Jahr Quelle:2022
Band/Heft Quelle:514(2022), 4, Seite 5751-5766
ISSN Quelle:1365-2966
Abstract:A comprehensive study of the co-evolution of globular cluster systems (GCS) in galaxies requires the ability to model both the large-scale dynamics (0.01-10 kpc) regulating their orbital evolution, and the small-scale dynamics (sub-pc - au) regulating the internal dynamics of each globular cluster (GC). In this work, we present a novel method that combine semi-analytic models of GCS with fully self-consistent Monte Carlo models to simultaneously evolve large GCSs. We use the population synthesis code MASinGa and the MOCCA-Survey Database I to create synthetic GC populations aimed at representing the observed features of GCs in the Milky Way (MW) and Andromeda (M31). Our procedure enables us to recover the spatial and mass distribution of GCs in such galaxies, and to constrain the amount of mass that GCs left either in the halo as dispersed debris, or in the galactic centre, where they can contribute to the formation of a nuclear star cluster (NSC) and can bring stellar and possibly intermediate mass black holes there. The final masses reported by our simulations are of a few order of magnitudes smaller than the observed values. These differences show that mass build-up of an NSC and central BHs in galaxies like MW and M31 cannot be solely explained by the infalling GC scenario. This build-up is likely to depend on the interplay between interactions and mergers of infalling GCs and gas. The latter can contribute to both in situ star formation in the NSC and growth of the central BH.
DOI:doi:10.1093/mnras/stac1694
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext ; Verlag: https://doi.org/10.1093/mnras/stac1694
 Volltext: https://www.webofscience.com/api/gateway?GWVersion=2&SrcAuth=DynamicDOIArticle&SrcApp=WOS&KeyAID=10.1093%2Fmnras%2Fstac1 ...
 DOI: https://doi.org/10.1093/mnras/stac1694
Datenträger:Online-Ressource
Sprache:eng
Sach-SW:color distributions
 early-type galaxies
 evolution
 galaxies: star clusters: general
 kinematics
 mass black-holes
 nuclear star-clusters
 origin
 parameters
 simulations
 systems
K10plus-PPN:1816708232
Verknüpfungen:→ Zeitschrift

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