\textunderscore Fermi-type particle acceleration from magnetic reconnection at the termination shock of relativistic striped wind
POSTER
Abstract
\textunderscore The termination shock of relativistic striped wind of obliquely rotating pulsars compresses the Poynting-flux-dominated flow and drives magnetic reconnection. Magnetic reconnection at the termination shock is highly efficient at converting magnetic energy into thermal energy and accelerating particles to high energies. By carrying out particle-in-cell simulations, we find that fermi-type mechanisms dominate the particle acceleration and power law formation. The maximum energy for electrons and positrons can reach hundreds of TeV if the wind has a Lorentz factor approximately 10\textasciicircum 6.
*Research presented in this paper was supported by the Center for Space and Earth Science (CSES) program and Laboratory Directed Research and Development (LDRD) program 20200367ER of Los Alamos National Laboratory (LANL). The simulations were performed with LANL Institutional Computing which is supported by the U.S. Department of Energy National Nuclear Security Administration under Contract No. 89233218CNA000001, and with the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation (NSF) grant number ACI-1548562.