Aspects of pulsar evolution

Fujimura, F. S.; Kennel, C. F.

doi:10.1086/157740

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-Cosmic Rays1

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1981

1988

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Cited by 11 publications

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“…e 10 10 g.cm y 7 and Ostriker, 1970;Fujimura and Kennel. 1980 ;s, 1980), T = initial spindown time = Ic /y 2 £L 2 , where T = pulsar lifetime (= time to cessation of pair creation?)…”

Section: -Cosmic Raysmentioning

confidence: 99%

Particle Acceleration by Pulsars

Arons

1981

Symp. - Int. Astron. Union

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The evidence that pulsars accelerate relativistic particles is reviewed, with emphasis on the γ-ray observations. The current state of knowledge of acceleration in strong waves is summarized, with emphasis on the inability of consistent theories to accelerate very high energy particles without converting too much energy into high energy photons. The state of viable models for pair creation by pulsars is summarized, with the conclusion that pulsars very likely lose rotational energy in winds instead of in superluminous strong waves. The relation of the pair creation models to γ-ray observations and to soft X-ray observations of pulsars is outlined, with the conclusion that energetically viable models may exist, but none have yet yielded useful agreement with the extant data. Some paths for overcoming present problems are discussed.

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“…e 10 10 g.cm y 7 and Ostriker, 1970;Fujimura and Kennel. 1980 ;s, 1980), T = initial spindown time = Ic /y 2 £L 2 , where T = pulsar lifetime (= time to cessation of pair creation?)…”

Section: -Cosmic Raysmentioning

confidence: 99%