Are There Two Pulsar Emission Mechanisms?

We show that ``core'' and ``cone'' pulsar emission profiles are connected, through standard theoretical models, to dynamical properties of the pulsar emission region. The models predict pair plasma formation only in pulsars which show core-type emission. Emission models which assume turbulence driven by relative velocities of the pair swarms probably apply to coral pulsars. If conal pulsars are pairless, however, a different emission mechanism is required for these objects.

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