2008/05/09 by R. Wunsch, Richard Wünsch, G. Tenorio‐Tagle +5 · 68 citations
Physics and Astronomy · #Astrophysics #Astrophysics and Star Formation Studies #Cluster (spacecraft) #Ejecta #Galaxy #Gamma-ray bursts and supernovae #Luminosity #Physics #RADIUS #Ram pressure #Star (game theory) #Star cluster #Star formation #Stars #Stellar, planetary, and galactic studies #Supernova #astro-ph
paper · pdf · doi:10.1086/589967
published in The Astrophysical Journal 683(2), 683-692 (IOP Publishing) · Accepted for publication in ApJ; 27 pages, 9 figures, 1 table
arxiv created 2008/05/09 · openalex publication_date 2008/08/19 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Using the hydrodynamic code ZEUS, we perform 2D simulations to determine the fate of the gas ejected by massive stars within super star clusters. It turns out that the outcome depends mainly on the mass and radius of the cluster. In the case of less massive clusters, a hot high velocity ( ∼ 1000 km s −1) stationary wind develops and the metals injected by supernovae are dispersed to large distances from the cluster. On the other hand, the density of the thermalized ejecta within massive and compact clusters is sufficiently large as to immediately provoke the onset of thermal instabilities. These deplete, particularly in the central densest regions, the pressure and the pressure gradient required to establish a stationary wind, and instead the thermally unstable parcels of gas are rapidly compressed, by a plethora of re-pressurizing shocks, into compact high density condensations. Most of these are unable to leave the cluster volume and thus accumulate to eventually feed further generations of star formation. 1