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arXiv · 2212.03226

Particle acceleration in shearing flows: the self-generation of turbulent spine-sheath structures in relativistic MHD jet simulations

Jie-Shuang Wang·Brian Reville·Yosuke Mizuno·Frank M. Rieger·Felix A. Aharonian
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Abstract

X-ray observations of several kiloparsec-scale extragalactic jets favour a synchrotron origin. The short cooling times of the emitting electrons requires distributed acceleration of electrons up to sub-PeV energies. In a previous paper, we found that this can be self-consistently explained by a shear acceleration model, where particles are accelerated to produce power-law spectra with a spectral index being determined mainly by the velocity profile and turbulence spectrum. In this paper, we perform 3D relativistic magneto-hydrodynamic simulations to investigate the formation of a spine-sheath structure and the development of turbulence for a relativistic jet propagating into a static cocoon. We explore different spine velocities and magnetic field profiles with values being chosen to match typical Fanaroff-Riley type I/II jets. We find that in all cases a sheath is generated on the interface of the spine and the cocoon mainly due to the Kelvin-Helmholtz instability. The large scale velocity profile in the sheath is close to linear. Turbulence develops in both the spine and the sheath, with a turbulent velocity spectrum consistent with Kolmogorov-scaling. The implications for shear particle acceleration are explored, with a focus on the particle spectral index.

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Jie-Shuang Wang, Brian Reville, Yosuke Mizuno, Frank M. Rieger, Felix A. Aharonian. 2022-12-06. Particle acceleration in shearing flows: the self-generation of turbulent spine-sheath structures in relativistic MHD jet simulations. https://doi.org/10.1093/mnras%2Fstac3616

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