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The Galactic Sources G5.4-1.2 and G5.27-0.90

Published online by Cambridge University Press:  04 August 2017

J.L. Caswell ,
M.J. Kesteven ,
R.F. Haynes ,
D.K. Milne ,
M.M. Komesaroff ,
R.T. Stewart  and
S.G. Wilson
J.L. Caswell
Affiliation:
Division of Radiophysics, CSIRO, PO Box 76, Epping, NSW 2121, Australia
M.J. Kesteven
Affiliation:
Division of Radiophysics, CSIRO, PO Box 76, Epping, NSW 2121, Australia
R.F. Haynes
Affiliation:
Division of Radiophysics, CSIRO, PO Box 76, Epping, NSW 2121, Australia
D.K. Milne
Affiliation:
Division of Radiophysics, CSIRO, PO Box 76, Epping, NSW 2121, Australia
M.M. Komesaroff
Affiliation:
Division of Radiophysics, CSIRO, PO Box 76, Epping, NSW 2121, Australia
R.T. Stewart
Affiliation:
Division of Radiophysics, CSIRO, PO Box 76, Epping, NSW 2121, Australia
S.G. Wilson
Affiliation:
Division of Radiophysics, CSIRO, PO Box 76, Epping, NSW 2121, Australia

Extract

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Long after a supernova event, the stellar core (neutron star) may continue to excite an extended remnant of ejecta surrounding it, as in the case of the Crab nebula. In contrast, the more common shell supernova remnants (SNRs) appear unaffected by any embedded neutron star.

Type
I. Rotation-Powered Pulsars
Information
Symposium - International Astronomical Union , Volume 125: The Origin and Evolution of Neutron Stars , 1987 , pp. 129
Copyright
Copyright © Reidel 1987