Abstract Based on the undisturbed finitely thick disk gravitational potential, 3-D trajectories of pulsars are followed with initial locations and velocities randomly selected from a model distribution. Three typical instances are followed for some 1011 yr, and their Poincaré sections are used as diagnostics of their motion. We find that the vertical-to-parallel range ratio (relative to the Galactic plane) to be an important parameter: as this ratio increases, the pulsar's motion changes from being regular to being irregular/chaotic.
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