2013/05/31 by Jan Palouš, Jan Palous, Richard Wunsch +6 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Cluster (spacecraft) #Computational astrophysics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Luminosity #RADIUS #Radiative cooling #Radiative transfer #Star cluster #Stellar mass #astro-ph.GA
paper · pdf · doi:10.1088/0004-637x/772/2/128
published as Astrophysical Journal, July 10, 2013, V771-2 · 21 pages, 6 figures, accepted to ApJ
arxiv created 2013/05/31 · openalex publication_date 2013/07/16 · arxiv updated 2015/06/16 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Hydrodynamic models for spherically symmetric winds driven by young stellar clusters with a generalized Schuster stellar density profile are explored. For this we use both semi-analytic models and one-dimensional numerical simulations. We determine the properties of quasi-adiabatic and radiative stationary winds and define the radius at which the flow turns from subsonic to supersonic for all stellar density distributions. Strongly radiative winds significantly diminish their terminal speed and thus their mechanical luminosity is strongly reduced. This also reduces their potential negative feedback into their host galaxy interstellar medium. The critical luminosity above which radiative cooling becomes dominant within the clusters, leading to thermal instabilities which make the winds non-stationary, is determined, and its dependence on the star cluster density profile, core radius, and half-mass radius is discussed.