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Structure of the Pulsar Magnetosphere

Published online by Cambridge University Press:  14 August 2015

L. Mestel*
Affiliation:
Astronomy Centre, University of Sussex

Extract

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Motivation for the study of the pulsar magnetosphere is multifold. First of all, energy-wise the magnetosphere is the dominant problem, for the energy emitted in the radio pulses is at most one per-cent of the energy loss inferred from the secular increase in the rotation period of the central neutron star. With the possible exception of gamma-ray emission in a few cases, the pulsing observed in all wavelengths can be regarded as a diagnostic of a more basic phenomenon. A successful model should in fact tell us the total rate of energy loss from the star and its distribution between a low-frequency wave, a possible wind, and emission in the radio, optical, X-ray and gamma-ray bands. As a necessary preliminary, the model should predict the strength of the currents leaving and returning to the star, the location of relativistic particles, and the conditions for transition to a quantum magnetosphere via pair production (Sturrock 1971). But even if magnetospheric theory did not offer such hopes of ultimate links with observation, the problem is so well-defined that it is a challenge to the theorist: it is just intolerable that we should not know how a rotating magnetized neutron star comes to terms with its environment.

Type
I. Electrodynamics of the Pulsar Magnetosphere and Wave Zone
Copyright
Copyright © Reidel 1981 

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