Physics
Scientific paper
Dec 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979ssrv...24..407k&link_type=abstract
(NASA and Jet Propulsion Laboratory, Workshop on the Physics of Planetary and Astrophysical Magnetospheres, Snowmass, Colo., Jul
Physics
37
Pulsar Magnetospheres, Pulsars, Stellar Atmospheres, Stellar Models, Coherent Radiation, Magnetic Flux, Magnetohydrodynamic Flow, Neutron Stars, Pair Production, Plasma Clouds, Relativistic Velocity, Stellar Envelopes, Stellar Mass, Stellar Motions, Vacuum Systems
Scientific paper
The structure of both the interior and exterior pulsar magnetosphere depends upon the strength of its plasma source near the surface of the star. We review magnetospheric models in the light of a vacuum pair-production source model proposed by Sturrock, and Ruderman and Sutherland. This model predicts the existence of a cutoff, determined by the neutron star's spin rate and magnetic field strength, beyond which coherent radio emission is no longer possible. The observed distribution of pulsar spin periods and period derivatives, and the distribution of pulsars with missing radio pulses, is quantitatively consistent with the pair production threshold, when its variation of neutron star radius and moment of inertia with mass is taken into account. All neutron stars observed as pulsars can have relativistic magnetohydrodynamic wind exterior magnetospheres. The properties of the wind can be directly related to those of the pair production source. Radio pulsars cannot have relativistic plasma wave exterior magnetospheres. On the other hand, most erstwhile pulsars in the galaxy are probably halo objects that emit weak fluxes of energetic photons that can have relativistic wave exterior magnetospheres. Extinct pulsars have not been yet observed.
Fujimura F. S.
Kennel Charles F.
Pellat Rene
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