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

被引：3

作者：

Badmaev, D. V. ^{[1
]}

Bykov, A. M. ^{[1
]}

Kalyashova, M. E. ^{[1
]}

机构：

[1] Ioffe Inst, 26 Politekhn Skaya St, St Petersburg 194021, Russia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 527卷 / 02期

关键词：

MHD; stars: winds; outflows; galaxies: star clusters: general; ISM: magnetic fields; ISM: supernova remnants; X-RAY-EMISSION; ION TEMPERATURE RATIO; STELLAR CLUSTERS; MAGNETIC-FIELD; WIND; REMNANTS; EVOLUTION; PLUTO; EXPLOSIONS; RADIATION;

D O I：

10.1093/mnras/stad3389

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 favourable for both proton and electron acceleration to energies well above TeV.

引用

页码：3749 / 3760

页数：12

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