1. Winds in Star Clusters Drive Kolmogorov Turbulence
- Author
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Enrico Ramirez-Ruiz, Anna L. Rosen, Blakesley Burkhart, Monica Gallegos-Garcia, and Jill Naiman
- Subjects
MHD TURBULENCE ,010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,CODE ,FOS: Physical sciences ,B stars ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,HYDRODYNAMICS ,Interstellar medium ,0103 physical sciences ,Cluster (physics) ,Astrophysics::Solar and Stellar Astrophysics ,INTERSTELLAR TURBULENCE ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Physics ,BUBBLES ,Turbulence ,Star formation ,NUMERICAL SIMULATIONS ,Isotropy ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Stars ,Star cluster ,GAS ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,SUPERNOVA FEEDBACK ,DENSITY ,Star clusters ,IONIZATION ,Astrophysics::Earth and Planetary Astrophysics ,Main sequence - Abstract
Intermediate and massive stars drive fast and powerful isotropic winds that interact with the winds of nearby stars in star clusters and the surrounding interstellar medium (ISM). Wind-ISM collisions generate astrospheres around these stars that contain hot $T\sim 10^7$ K gas that adiabatically expands. As individual bubbles expand and collide they become unstable, potentially driving turbulence in star clusters. In this paper we use hydrodynamic simulations to model a densely populated young star cluster within a homogeneous cloud to study stellar wind collisions with the surrounding ISM. We model a mass-segregated cluster of 20 B-type young main sequence stars with masses ranging from 3--17 $M_{\odot}$. We evolve the winds for $\sim$11 kyrs and show that wind-ISM collisions and over-lapping wind-blown bubbles around B-stars mixes the hot gas and ISM material generating Kolmogorov-like turbulence on small scales early in its evolution. We discuss how turbulence driven by stellar winds may impact the subsequent generation of star formation in the cluster, 12 pages, 5 figures, Accepted for publication in ApJL
- Published
- 2020
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