Hydrodynamic simulation of Cygnus OB2

• Verfasst von: Vieu, Thibault [VerfasserIn]
• Verfasst von: Larkin, Cormac [VerfasserIn]
• Verfasst von: Härer, L. [VerfasserIn]
• Verfasst von: Reville, Brian [VerfasserIn]
• Verfasst von: Sander, Andreas A. C. [VerfasserIn]
• Verfasst von: Ramachandran, Varsha [VerfasserIn]
• Titel: Hydrodynamic simulation of Cygnus OB2
• Titelzusatz: the absence of a cluster wind termination shock
• Verf.angabe: T. Vieu, C.J.K. Larkin, L. Härer, B. Reville, A.A.C. Sander and V. Ramachandran
• E-Jahr: 2024
• Jahr: August 2024
• Umfang: 15 S.
• Fussnoten: Online veröffentlicht: 2. Juli 2024 ; Gesehen am 03.12.2024
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2024
• Band/Heft Quelle: 532(2024), 2 vom: Aug., Seite 2174-2188
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stae1627
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1910684120

Abstract

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.