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dc.contributor.authorRadhakrishnan, V.-
dc.contributor.authorSrinivasan, G.-
dc.identifier.citationJournal of Astrophysics and Astronomy, 1980, Vol. 1, p25-32.en
dc.description.abstractWe use the recently introduced concept of a ' window ' of magnetic field strengths in which pulsars can be active to explain the variation in morphology of supernova remnants. The striking difference between shell-type and filled-type remnants is attributed to differences in the magnetic field strengths of the neutron stars left by the respective supernovae. Field strengths of a value permitting pulsar activity result in particle production and Crab-like centrally concentrated remnants. Other field values lead to strong magnetic dipole radiation and consequent shell formation (e.g. Cas A). Several apparent inconsistencies concerning pulsar-supernova associations appear to find a logical explanation on the basis of this hypothesis.en
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dc.publisherIndian Academy of Sciences, Bangalore, India.en
dc.rightsIndian Academy of Sciences, Bangalore, India.en
dc.subjectSupernova remnantsen
dc.subjectMagnetic windowen
dc.titlePulsar activity and the morphology of supernova remnantsen
Appears in Collections:Research Papers (A&A)

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