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Using the three-dimensional relativistic magnetohydrodynamic code RAISHIN, weinvestigated the influence of radial density profile on the spatial developmentof the current-driven kink instability along magnetized rotating, relativisticjets. For the purpose of our study, we used a non-periodic computational box,the jet flow is initially established across the computational grid, and aprecessional perturbation at the inlet triggers the growth of the kinkinstability. We studied light as well as heavy jets with respect to theenvironment depending on the density profile. Different angular velocityamplitudes have been also tested. The results show the propagation of ahelically kinked structure along the jet and relatively stable configurationfor the lighter jets. The jets appear to be collimated by the magnetic fieldand the flow is accelerated due to conversion of electromagnetic into kineticenergy. We also identify regions of high current density in filamentary currentsheets, indicative of magnetic reconnection, which are associated to the kinkunstable regions and correlated to the decrease of the sigma parameter of theflow. We discuss the implications of our findings for Poynting-flux dominatedjets in connection with magnetic reconnection process. We find that fastmagnetic reconnection may be driven by the kink-instability turbulence andgovern the transformation of magnetic into kinetic energy thus providing anefficient way to power and accelerate particles in AGN and gamma-ray-burstrelativistic jets.

Spatial growth of current-driven instability in relativistic rotating jets and the search for magnetic reconnection