2023MNRAS.522.4238M

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.