Core-collapse supernova inside the core of a young massive star cluster: 3D MHD simulations

Abstract

Young massive stars in compact stellar clusters could end their evolution as core-collapse supernovae a few million years after the cluster was built. The blast wave of a supernova propagates through the inner cluster region with multiple stellar winds of young luminous stars. We present the results of 3D magnetohydrodynamic simulations of the plasma flows produced by a supernova event inside a cluster with a population of massive stars similar to that in Westerlund 1. We followed its evolution over a few thousand years (i.e. a few shock crossing times). The plasma temperature, density and magnetic field, which are highly disturbed by supernova event, relax to values close to the initial over the studied period. The relaxation time of a cluster is a few thousand years, which is a sizeable fraction of the period between the successive supernova events for a massive cluster of a few million years age. The spectra of the cluster diffuse X-ray emission simulated here should be representative for the galactic and extragalactic young massive clusters. The resultant magnetic fields are highly intermittent, so we derived the volume filling factors for a set of magnetic field ranges. Highly amplified magnetic fields of magnitude well above 100 $\mu$G fill in a few per cent of the cluster volume, but still dominate the magnetic energy. The structure of the magnetic fields and high velocity plasma flows with shocks in the system are favorable for both proton and electron acceleration to energies well above TeV.

12 pages, 11 figures; accepted to MNRAS

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Cited by in corpus (4)

• Very-high-energy $\gamma$-ray emission from young massive star clusters in the Large Magellanic Cloud
• Stellar-wind feedback and magnetic fields around young compact star clusters: 3D MHD simulations
• How interacting winds shape the mechanical feedback of massive star clusters over millions of years
• Direct simulations of very high energy cosmic ray acceleration in 3D MHD model of a compact star cluster