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Hydrodynamic simulation of Cygnus OB2: the absence of a cluster wind termination shock

ABSTRACT -We perform a large-scale hydrodynamic simulation of a massive star cluster whose stellar population mimics that of the Cygnus OB2 association. The main-sequence stars are first simulated during 1.6 Myr, until a quasi-stationary state is reached. At this time, the three Wolf-Rayet stars obs...

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Main Authors: Vieu, Thibault (Author) , Larkin, Cormac (Author) , Härer, L. (Author) , Reville, Brian (Author) , Sander, Andreas A. C. (Author) , Ramachandran, Varsha (Author)
Format: Article (Journal)
Language:English
Published: August 2024
In: Monthly notices of the Royal Astronomical Society
Year: 2024, Volume: 532, Issue: 2, Pages: 2174-2188
ISSN:1365-2966
DOI:10.1093/mnras/stae1627
Online Access:Verlag, kostenfrei, Volltext: https://doi.org/10.1093/mnras/stae1627
Verlag, kostenfrei, Volltext: https://academic.oup.com/mnras/article/532/2/2174/7704458
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Author Notes:T. Vieu, C.J.K. Larkin, L. Härer, B. Reville, A.A.C. Sander and V. Ramachandran
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Summary:ABSTRACT -We perform a large-scale hydrodynamic simulation of a massive star cluster whose stellar population mimics that of the Cygnus OB2 association. The main-sequence stars are first simulated during 1.6 Myr, until a quasi-stationary state is reached. At this time, the three Wolf-Rayet stars observed in Cygnus OB2 are added to the simulation, which continues to 2 Myr. Using a high-resolution grid in the centre of the domain, we can resolve the most massive stars individually, which allows us to probe the kinetic structures at small (parsec) scales. We find that, although the cluster excavates a spherical ‘superbubble’ cavity, the stellar population is too loosely distributed to blow a large-scale cluster wind termination shock, and that collective effects from wind-wind interactions are much less efficient than usually assumed. This challenges our understanding of the ultra-high energy emission observed from the region.
Item Description:Online veröffentlicht: 2. Juli 2024
Gesehen am 03.12.2024
Physical Description:Online Resource
ISSN:1365-2966
DOI:10.1093/mnras/stae1627

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