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STIRRED, NOT SHAKEN: STAR CLUSTER SURVIVAL IN THE SLINGSHOT SCENARIO

D R Matus Carrillo,
D R Matus Carrillo
Departamento de Astronomía, Universidad de Concepción
, Casilla 160-C, Concepción,
Chile
E-mail: dimatus@udec.cl
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M Fellhauer,
M Fellhauer
Departamento de Astronomía, Universidad de Concepción
, Casilla 160-C, Concepción,
Chile
  https://orcid.org/0000-0002-3989-4115
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T C N Boekholt,
T C N Boekholt
Rudolf Peierls Centre for Theoretical Physics, Clarendon Laboratory
, Parks Road, Oxford, OX1 3PU,
UK
  https://orcid.org/0000-0002-6911-6584
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A Stutz,
A Stutz
Departamento de Astronomía, Universidad de Concepción
, Casilla 160-C, Concepción,
Chile
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M C B Morales Inostroza
M C B Morales Inostroza
Departamento de Astronomía, Universidad de Concepción
, Casilla 160-C, Concepción,
Chile
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Monthly Notices of the Royal Astronomical Society, stad1256,
https://doi.org/10.1093/mnras/stad1256
Published:
27 April 2023

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   D R Matus Carrillo, M Fellhauer, T C N Boekholt, A Stutz, M C B Morales
   Inostroza, Stirred, not shaken: Star cluster survival in the slingshot
   scenario, Monthly Notices of the Royal Astronomical Society, 2023;, stad1256,
   https://doi.org/10.1093/mnras/stad1256
   
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ABSTRACT

We investigate the effects of an oscillating gas filament on the dynamics of its
embedded stellar clusters. Motivated by recent observational constraints, we
model the host gas filament as a cylindrically symmetrical potential, and the
star cluster as a Plummer sphere. In the model, the motion of the filament will
produce star ejections from the cluster, leaving star cluster remnants that can
be classified into four categories: a) Filament Associated clusters, which
retain most of their particles (stars) inside the cluster and inside the
filament; b) destroyed clusters, where almost no stars are left inside the
filament, and there is no surviving bound cluster; c) ejected clusters, that
leave almost no particles in the filament, since the cluster leaves the gas
filament; and d) transition clusters, corresponding to those clusters that
remain in the filament, but that lose a significant fraction of particles due to
ejections induced by filament oscillation. Our numerical investigation predicts
that the Orion Nebula Cluster is in the process of being ejected, after which it
will most likely disperse into the field. This scenario is consistent with
observations which indicate that the Orion Nebula Cluster is expanding, and
somewhat displaced from the Integral Shaped Filament ridgeline.

stars: kinematics and dynamics, ISM: individual objects, methods: numerical
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articles, which may therefore contain changes. The DOI will remain the same
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© 2023 The Author(s) Published by Oxford University Press on behalf of Royal
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