Cosmic ray acceleration and scattering in a 3D MHD model of compact massive star clusters

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Abstract

Compact young massive star clusters (YMSCs) contain dozens ofO-, B-, andWR-type stars with powerful, fast winds within a radius of ∼1 pc. In the turbulent environment of such clusters, particle acceleration by ensembles of shock waves and compression/rarefaction waves is possible. This work investigates the propagation and acceleration of particles in YMSCs using three-dimensional magnetohydrodynamic (MHD) simulations with the open source code PLUTO and its built-in module for solving the equations of motion for test charged particles. It is found that in the cluster core, near the termination shocks ofO-star winds, as well as at the collective wind termination shock, protons are accelerated to energies ≳100 TeV. The spatial and energy distributions of the particles are discussed.

About the authors

M. E. Kalyashova

Ioffe Institute

Email: m.kalyashova@gmail.com
Saint Petersburg

A. M. Bykov

Ioffe Institute

Email: byk@astro.ioffe.ru
Saint Petersburg

D. V. Badmaev

Ioffe Institute

Email: danirbadmaev.astro@gmail.com
Saint Petersburg

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