English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

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

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