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Pulsar Activity and Supernova Remnant Morphology

Published online by Cambridge University Press:  14 August 2015

V. Radhakrishnan  and
G. Srinivasan
V. Radhakrishnan
Affiliation:
Raman Research Institute, Bangalore-560 080, India
G. Srinivasan
Affiliation:
Raman Research Institute, Bangalore-560 080, India

Abstract

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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. Neutron stars created with 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.

Type
IX. Pulsars and Supernovae
Information
Symposium - International Astronomical Union , Volume 95: Pulsars , 1981 , pp. 417 - 419
Copyright
Copyright © Reidel 1981 

References

Ostriker, J. P. and Gunn, J. E.: 1971, Astrophys. J. Letters 164, pp. L95–104.Google Scholar
Radhakrishnan, V.: 1980, in: Non Solar Gamma-Rays (COSPAR), eds.: Cowsik, R. and Wills, R. D., Pergamon Press, Oxford, pp. 163–174.Google Scholar
Shklovskii, I. S.: 1978, Sov. Astron. 22, pp. 413–420.Google Scholar
Shukre, C. S. and Radhakrishnan, V.: 1980, submitted to Astrophys. J.Google Scholar
Weiler, K. W. and Panagia, N.: 1978, Astron. Astrophys. 70, pp. 419–422.Google Scholar