3D PIC Simulations for Relativistic Jets with a Toroidal Magnetic Field. (arXiv:2009.04158v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Meli_A/0/1/0/all/0/1">A. Meli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nishikawa_K/0/1/0/all/0/1">K. Nishikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pohl%2E_M/0/1/0/all/0/1">M. Pohl.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niemiec_J/0/1/0/all/0/1">J. Niemiec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dutan_I/0/1/0/all/0/1">I. Dutan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koehn_C/0/1/0/all/0/1">C. Koehn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mizuno_Y/0/1/0/all/0/1">Y. Mizuno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacDonald_N/0/1/0/all/0/1">N. MacDonald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_J/0/1/0/all/0/1">J. L. Gomez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirotani_K/0/1/0/all/0/1">K. Hirotani</a>
The properties of relativistic jets, their interaction with the ambient
environment, and particle acceleration due to kinetic instabilities are studied
self-consistently with Particle-in-Cell simulations. An important key issue is
how a toroidal magnetic field affects the evolution of an e$^{pm}$ and an
e$^{-}$ – p$^{+}$ jet, how kinetic instabilities such as the Weibel instability
(WI), the mushroom instability (MI) and the kinetic Kelvin-Helmholtz
instability (kKHI) are excited, and how such instabilities contribute to
particle acceleration. We show that WI, MI and kKHI excited at the linear
stage, generate a quasi-steady $x$-component of electric field which
accelerates and decelerates electrons. In this work, we use a new jet injection
scheme where an electric current is self-consistently generated at the jet
orifice by the jet particles. We inject both e$^{pm}$ and e$^{-}$ – p$^{+}$
jets with a toroidal magnetic field (with a top-hat jet density profile) and
for a sufficiently long time in order to examine the non-linear effects of the
jet evolution. Despite the weakness of the initial magnetic field, we observe
significant differences in the structure of the strong electromagnetic fields
that are driven by the kinetic instabilities. We find that different jet
compositions present different strongly excited instability modes. The magnetic
field in the non-linear stage generated by different instabilities becomes
dissipated and reorganized into a new topology. The 3-dimensional magnetic
field topology indicates possible reconnection sites and the accelerated
particles are significantly accelerated in the non-linear stage by the
dissipation of the magnetic field and/or reconnection. This study will shed
further light on the nature of astrophysical relativistic magnetized jet
phenomena.
The properties of relativistic jets, their interaction with the ambient
environment, and particle acceleration due to kinetic instabilities are studied
self-consistently with Particle-in-Cell simulations. An important key issue is
how a toroidal magnetic field affects the evolution of an e$^{pm}$ and an
e$^{-}$ – p$^{+}$ jet, how kinetic instabilities such as the Weibel instability
(WI), the mushroom instability (MI) and the kinetic Kelvin-Helmholtz
instability (kKHI) are excited, and how such instabilities contribute to
particle acceleration. We show that WI, MI and kKHI excited at the linear
stage, generate a quasi-steady $x$-component of electric field which
accelerates and decelerates electrons. In this work, we use a new jet injection
scheme where an electric current is self-consistently generated at the jet
orifice by the jet particles. We inject both e$^{pm}$ and e$^{-}$ – p$^{+}$
jets with a toroidal magnetic field (with a top-hat jet density profile) and
for a sufficiently long time in order to examine the non-linear effects of the
jet evolution. Despite the weakness of the initial magnetic field, we observe
significant differences in the structure of the strong electromagnetic fields
that are driven by the kinetic instabilities. We find that different jet
compositions present different strongly excited instability modes. The magnetic
field in the non-linear stage generated by different instabilities becomes
dissipated and reorganized into a new topology. The 3-dimensional magnetic
field topology indicates possible reconnection sites and the accelerated
particles are significantly accelerated in the non-linear stage by the
dissipation of the magnetic field and/or reconnection. This study will shed
further light on the nature of astrophysical relativistic magnetized jet
phenomena.
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