Correlating Particle Acceleration Rates with Plasma Conditions in Colliding Wind Binaries

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ID: 318004
2026
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Abstract
Abstract Recent observations have revealed star-forming regions as possible origin sites of very-high-energy (TeV) cosmic rays, not associated with supernova remnants. Colliding-wind binaries are strong X-ray and radio synchrotron emitters and have been proposed as potential accelerators of such particles. We perform high-resolution three-dimensional magnetohydrodynamic simulations coupled with test-particle integration to investigate how local plasma conditions affect particle acceleration in wind-wind collisions. We find that the maximum particle energies and the hardness of the energy distributions depend on the shock magnetization and cooling efficiency. For moderate magnetization (>1 G), CWBs can accelerate hadronic particles up to hundreds of TeV or even PeV energies, with more than 1 per cent of particles reaching the > TeV energy range. By correlating the local acceleration rate with plasma quantities — magnetic field strength, current density, vorticity, and velocity divergence — we show that turbulence and magnetic field complexity dominate the acceleration, while classical diffusive shock acceleration plays a limited role. These results suggest that turbulent, magnetically driven processes are key to producing relativistic particles in CWBs, with implications for future high sensitivity γ-ray observations (e.g. LACT and CTAO).
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Authors Gislaine B Cordeiro, D. Falceta-Gonçalves, G. Kowal, Vanessa Giraldez-Garcia
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1154
URL
https://doi.org/10.1093/mnras/stag1154
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