Stirred, not shaken: star cluster survival in the slingshot scenario
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 th...
| Main Authors: | , , , , |
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| Format: | Journal article |
| Language: | English |
| Published: |
Oxford University Press
2023
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| _version_ | 1797109918352801792 |
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| author | Carrillo, DRM Fellhauer, M Boekholt, TCN Stutz, A Inostroza, MCBM |
| author_facet | Carrillo, DRM Fellhauer, M Boekholt, TCN Stutz, A Inostroza, MCBM |
| author_sort | Carrillo, DRM |
| collection | OXFORD |
| description | 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. |
| first_indexed | 2024-03-07T07:47:54Z |
| format | Journal article |
| id | oxford-uuid:10b23b4d-dfbd-4c6d-bb8b-0dee66d64265 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T07:47:54Z |
| publishDate | 2023 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:10b23b4d-dfbd-4c6d-bb8b-0dee66d642652023-06-27T11:15:16ZStirred, not shaken: star cluster survival in the slingshot scenarioJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:10b23b4d-dfbd-4c6d-bb8b-0dee66d64265EnglishSymplectic ElementsOxford University Press2023Carrillo, DRMFellhauer, MBoekholt, TCNStutz, AInostroza, MCBMWe 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. |
| spellingShingle | Carrillo, DRM Fellhauer, M Boekholt, TCN Stutz, A Inostroza, MCBM Stirred, not shaken: star cluster survival in the slingshot scenario |
| title | Stirred, not shaken: star cluster survival in the slingshot scenario |
| title_full | Stirred, not shaken: star cluster survival in the slingshot scenario |
| title_fullStr | Stirred, not shaken: star cluster survival in the slingshot scenario |
| title_full_unstemmed | Stirred, not shaken: star cluster survival in the slingshot scenario |
| title_short | Stirred, not shaken: star cluster survival in the slingshot scenario |
| title_sort | stirred not shaken star cluster survival in the slingshot scenario |
| work_keys_str_mv | AT carrillodrm stirrednotshakenstarclustersurvivalintheslingshotscenario AT fellhauerm stirrednotshakenstarclustersurvivalintheslingshotscenario AT boekholttcn stirrednotshakenstarclustersurvivalintheslingshotscenario AT stutza stirrednotshakenstarclustersurvivalintheslingshotscenario AT inostrozamcbm stirrednotshakenstarclustersurvivalintheslingshotscenario |