TY - JOUR
T1 - Winds in Star Clusters Drive Kolmogorov Turbulence
AU - Gallegos-Garcia, Monica
AU - Burkhart, Blakesley
AU - Rosen, Anna L.
AU - Naiman, Jill P.
AU - Ramirez-Ruiz, Enrico
N1 - Publisher Copyright:
© 2020. The American Astronomical Society. All rights reserved.
PY - 2020/8
Y1 - 2020/8
N2 - 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 ∼ 107 K gas that adiabatically expands. As individual bubbles expand and collide they become unstable, potentially driving turbulence in star clusters. In this Letter 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 to 17 M o˙. We evolve the winds for ∼11 kyr and show that wind-ISM collisions and overlapping wind-blown bubbles around B-stars mix 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.
AB - 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 ∼ 107 K gas that adiabatically expands. As individual bubbles expand and collide they become unstable, potentially driving turbulence in star clusters. In this Letter 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 to 17 M o˙. We evolve the winds for ∼11 kyr and show that wind-ISM collisions and overlapping wind-blown bubbles around B-stars mix 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.
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U2 - 10.3847/2041-8213/ababae
DO - 10.3847/2041-8213/ababae
M3 - Article
AN - SCOPUS:85090468980
SN - 2041-8205
VL - 899
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 2
M1 - L30
ER -