Phenomenological pulsar model

We adopt particle injection energies and rates previously claculated for the stellar wind generation by rotating magnetized neutron stars. We assume that the ambient space-charge density being emitted to form this wind is bunched. These considerations immediately place the coherent radio frequency luminosity from such bunches at around 1028 ergs s-1 for typical pulsar parameters. A comparable amount of incoherent radiation is emitted for typical (1 second) pulsars. For very rapid pulsars, however, the latter component grows more rapidly than the available energy sources. We attribute the comparatively low radio luminosity of the Crab and Vela pulsars to both components being limited in the same ratio. The incoherent radiation essentially has a synchrotron spectrum and extends to γ-ray energies; consequently the small part of the total luminosity that is at optical wavelengths is unobservable. Assuming full coherence at all wavelengths short of a critical length gives a spectral index for the flux density of -8/3 at higher frequencies. The finite energy available from the injected particles would force the spectrum to roll over below about 100 MHz (as typically observed), although intrinsic morphological factors probably enter (e.g., scale of field inhomogeneities at the surface) for any specific pulsar as well