Kinetic Simulations of Instabilities in Cylindrical Magnetized Jets

José Ortuño-Macı́as and Krzysztof Nalewajko

High-energy astrophysical phenomena commonly involve regions with magnetic energy density that locally dominates the rest-mass energy density of matter. Such relativistic magnetizations can be converted to relativistic particle acceleration, which is observed in the form of luminous non-thermal emission with photon energies extending into the gamma-ray band. Relativistically magnetized regions are expected in the relativistic jets, which may involve ordered magnetic fields with poloidal and toroidal components, the latter prone to the m = 0 pinch and m = 1 kink instability modes (Begelman, 1998). Recently, the first 3D kinetic numerical simulations of cylindrical magnetized columns reported efficient particle acceleration in two different magnetic field configurations, with the toroidal field supported either by the poloidal field (Davelaar et al., 2020) or by the gas pressure (Alves et al., 2018). Here we report preliminary results from our 3D kinetic simlations of cylindrical magnetized columns with the toroidal field supported by a combination of poloidal field and gas pressure.

Proceedings of the Polish Astronomical Society, vol. 12, 241-243 (2022)

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