Wind of a young massive star colliding with a supernova remnant shell

Badmaev, D. V.; Bykov, A. M.

doi:10.1088/1742-6596/2103/1/012013

Cited by 2 publications

(1 citation statement)

References 34 publications

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“…Additionally, collisions between supernova remnants and stellar winds from nearby massive stars have been simulated using both hydrodynamic and MHD models (e.g. Badmaev & Bykov 2021;Velázquez et al 2003Velázquez et al , 2023.…”

Section: Introductionmentioning

confidence: 99%

Inside the core of a young massive star cluster: 3D MHD simulations

Badmaev

Bykov

Kalyashova

2022

Monthly Notices of the Royal Astronomical Society

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Young massive star clusters inhabit regions of star formation and play an essential role in the galactic evolution. They are sources of both thermal and non-thermal radiation, and they are effective cosmic ray accelerators. We present the 3D magnetohydrodynamic (MHD) modeling of the plasma flows in a young compact cluster at the evolutionary stage comprising multiple interacting supersonic winds of massive OB and WR stars. The modeling allows studying the partitioning of the mechanical energy injected by the winds between the bulk motions, thermal heating and magnetic fields. Cluster-scale magnetic fields reaching the magnitudes of ∼ 300 μG show the filamentary structures spreading throughout the cluster core. The filaments with the high magnetic fields are produced by the Axford-Cranfill type effect in the downstream of the wind termination shocks, which is amplified by a compression of the fields with the hot plasma thermal pressure in the central part of the cluster core. The hot (∼ a few keV) plasma is heated at the termination shocks of the stellar winds and compressed in the colliding postshock flows. We also discuss a possible role of the thermal conduction effects on the plasma flow, analyse temperature maps in the cluster core and the diffuse thermal X-ray emission spectra. The presence of high cluster-scale magnetic fields supports the possibility of high-energy cosmic ray acceleration in clusters at the given evolutionary stage.

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Section: Introductionmentioning

confidence: 99%

Inside the core of a young massive star cluster: 3D MHD simulations

Badmaev

Bykov

Kalyashova

2022

Monthly Notices of the Royal Astronomical Society

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

Badmaev,

Bykov,

Kalyashova

2023

Monthly Notices of the Royal Astronomical Society

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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 µG 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.

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Wind of a young massive star colliding with a supernova remnant shell

Cited by 2 publications

References 34 publications

Inside the core of a young massive star cluster: 3D MHD simulations

Inside the core of a young massive star cluster: 3D MHD simulations

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

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