Pulsar activity and the morphology of supernova remnants

dc.contributor.author	Radhakrishnan, V
dc.contributor.author	Srinivasan, G
dc.date.accessioned	2005-12-29T04:54:10Z
dc.date.available	2005-12-29T04:54:10Z
dc.date.issued	1980
dc.description.abstract	We 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
dc.format.extent	848912 bytes
dc.format.mimetype	application/pdf
dc.identifier.citation	Journal of Astrophysics and Astronomy, 1980, Vol. 1, p25-32.	en
dc.identifier.issn	0250-6335
dc.identifier.uri	http://hdl.handle.net/2289/943
dc.language.iso	en	en
dc.publisher	Indian Academy of Sciences, Bangalore, India.	en
dc.rights	Indian Academy of Sciences, Bangalore, India.	en
dc.subject	Pulsars	en
dc.subject	Supernova remnants	en
dc.subject	Magnetic window	en
dc.title	Pulsar activity and the morphology of supernova remnants	en
dc.type	Article	en

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