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Neutrinos drive core-collapse supernovae, launch outflows from neutron starmerger accretion disks, and set the ratio of protons to neutrons in ejecta fromboth systems that generate heavy elements in the universe. Neutrinos ofdifferent flavors interact with matter differently, and much recent work hassuggested that fast flavor instabilities are likely ubiquitous in both systems,but the final flavor content after the instability saturates has not been wellunderstood. In this work we present particle-in-cell calculations which followthe evolution of all flavors of neutrinos and antineutrinos through saturationand kinematic decoherence. We conduct one-dimensional three-flavor simulationsof neutrino quantum kinetics to demonstrate the outcome of this instability ina few example cases. We demonstrate the growth of both axially symmetric andasymmetric modes whose wavelength and growth rate match predictions from linearstability analysis. Finally, we vary the number density, flux magnitude, andflux direction of the neutrinos and antineutrinos and demonstrate that thesefactors modify both the growth rate and post-saturation neutrino flavorabundances. Weak electron lepton number (ELN) crossings in these simulationsproduce both slow growth of the instability and little difference between theflavor abundances in the initial and final states. In all of these calculationsthe same number of neutrinos and antineutrinos change flavor, making the leastabundant between them the limiting factor for post-saturation flavor change.Many more simulations and multi-dimensional simulations are needed to fullyprobe the parameter space of the initial conditions.

Particle-in-cell Simulation of the Neutrino Fast Flavor Instability