Stirred, not shaken: Star cluster survival in the slingshot scenario

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.

13 pages, 17 figures

References in corpus (11)

• Using the minimum spanning tree to trace mass segregation
• A multiphysics and multiscale software environment for modeling astrophysical systems
• On the Structure of the Orion A Cloud and the Formation of the Orion Nebula Cluster
• Kinematic Structure of the Orion Nebula Cluster and its Surroundings
• Evolution of column density distributions within Orion~A
• IN-SYNC II: Virial Stars from Sub-Virial Cores -- The Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333
• A Tale of Three Cities: OmegaCAM discovers multiple sequences in the color-magnitude diagram of the Orion Nebula Cluster
• The Structure, Dynamics and Star Formation Rate of the Orion Nebula Cluster
• Evidence for Radial Expansion at the Core of the Orion Complex with Gaia EDR3
• The 3-D Kinematics of the Orion Nebula Cluster: NIRSPEC-AO Radial Velocities of the Core Population
• The Core Mass Function in the Orion Nebula Cluster Region: What Determines the Final Stellar Masses?

Cited by in corpus (2)

• The 3D Kinematics of the Orion Nebula Cluster II: Mass-dependent Kinematics of the Inner Cluster
• Massive star cluster formation III. Early mass segregation during cluster assembly