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The electromagnetic emission from neutron star mergers is comprised ofmultiple components. Synchrotron emission from the disk-powered jet as well asthermal emission from the merger ejecta (powered by a variety of sources) areamong the most studied sources. The low masses and high velocities of themerger ejecta quickly develop conditions where emission from collisionlessshocks becomes critical and synchrotron emission from the merger ejectaconstitutes a third component to the observed signal. The aim of this projectis to examine shock development, magnetic field generation and particleacceleration in the case of mildly relativistic shocks, which are expected whenthe tidal ejecta of neutron star mergers drive a shock into the externalmedium. Using LANL's VPIC (vector particle-in-cell) code, we have runsimulations of such mildly-relativistic, collisionless, weakly-magnetizedplasmas and compute the resultant magnetic fields and particle energy spectra.We show the effects of varying plasma conditions, as well as explore thevalidity of using different proton to electron mass ratios in VPIC. Our resultshave implications for observing late-time electromagnetic counterparts togravitational wave detections of neutron star mergers.

Particle In Cell Simulations of Mildly Relativistic Outflows in Kilonova Emissions