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30 Doradus, the double stellar birth scenario by N-body & warpfield clouds

We study the evolution of embedded star clusters as possible progenitors to reproduce 30 Doradus, specifically the compact star cluster known as R136 and its surrounding stellar family, which is believed to be part of an earlier star formation event. We employ the high-precision stellar dynamics cod...

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Hauptverfasser: Dominguez, Raul (VerfasserIn) , Pellegrini, Eric William (VerfasserIn) , Klessen, Ralf S. (VerfasserIn) , Rahner, Daniel (VerfasserIn)
Dokumenttyp: Article (Journal) Kapitel/Artikel
Sprache:Englisch
Veröffentlicht: 13 May 2022
In: Arxiv
Year: 2022, Pages: 1-13
DOI:10.48550/arXiv.2205.06209
Online-Zugang:Verlag, lizenzpflichtig, Volltext: https://doi.org/10.48550/arXiv.2205.06209
Verlag, lizenzpflichtig, Volltext: http://arxiv.org/abs/2205.06209
Volltext
Verfasserangaben:R. Domínguez, Eric W. Pellegrini, Ralf S. Klessen, Daniel Rahner
Beschreibung
Zusammenfassung:We study the evolution of embedded star clusters as possible progenitors to reproduce 30 Doradus, specifically the compact star cluster known as R136 and its surrounding stellar family, which is believed to be part of an earlier star formation event. We employ the high-precision stellar dynamics code NBODY6++GPU to calculate the dynamics of the stars embedded in different evolving molecular clouds modelled by the 1D cloud/clusters evolution code WARPFIELD. We explore clouds with initial masses of $M_\text{cloud}=3.16 \times 10^{5}$ M$_\odot$ that (re)-collapse allowing for the birth of a second generation of stars. We explore different star formation efficiencies in order to find the best set of parameters that can reproduce the observation measurements. Our best-fit models correspond to a first stellar generation with masses between $1.26 \times 10^4$ - $2.85 \times 10^4 $M$_\odot$ and for the second generation we find a
Beschreibung:Version 1 vom 12 Mai 2022, Version 2 vom 13 Mai 2022
Im Titel wird "Warpfield" groß geschrieben
Gesehen am 17.10.2022
Beschreibung:Online Resource
DOI:10.48550/arXiv.2205.06209

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