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Center for Nonlinear Studies |
Recent large scale Particle-in-Cell (PIC) simulations have demonstrated that in relativistic electron-ion shear flows, ordered transverse magnetic fields are created by current sheets on opposite sides of the shear interface. Instead of dissipating the shear flow energy via turbulence as in MHD simulations, relativistic kinetic shear flow stabilizes itself via the formation of a robust ion vacuum gap supported by the self-generated magnetic field, which effectively separates the opposing ion flows with no mixing. This strongly magnetized shear boundarylayer appears stable, lasting many tens of light crossing times of the simulation box. Electrons are energized to reach the ion kinetic energy, with the highest energy electrons following looping trajectories along the shear interface and emitting narrowly beamed radiation. Here we discuss the application of the PIC simulation results to model the radiation of jets created by neutron star merger events such as GW170817/GRB170817A.
Host: Timothy Waters