Relativistic jets emit large quantities of electromagnetic radiation, yet the mechanism for this emission is not agreed upon. Using 3D general relativistic magnetohydrodynamic (GRMHD) simulations of black hole accretion, we investigate the origin of this emission. For the first time, simulations of toroidal magnetic field show flips in polarity of magnetic flux on the black hole. Such flips lead to current sheets within the jet, which dissipate magnetic energy into heat and radiation. By measuring the time between the flips we aim to predict the distance at which the dissipation will occur.
Based on research done by Emma Kaufman, Ian Christie, Aris Lalakos, and Alexander Tchekhovskoy.