Abstract
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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