 |
Center for Nonlinear Studies |
Magnetic reconnection regions have long been expected to be sources of high-energy particles. Recent observations of planetary magnetotails, solar flares and gamma-ray flares from the Crab nebula have motivated us to better understand magnetic reconnection and its associated particle acceleration. However, the multi-scale nature of the problem makes it challenging to model numerically. I will present 2D and 3D fully kinetic simulations of magnetic reconnection in the highly magnetized regime (plasma beta << 1). This includes the new VPIC simulations on LANL’s Trinity machine. Quite robustly, the simulation results show that the magnetic energy is converted efficiently into kinetic energy of nonthermal relativistic particles in a power-law spectrum. I will discuss our new understandings on several key issues including the main acceleration mechanism, the formation of power-law distribution, and the effect of 3D turbulence on the production of nonthermal particles.