Hostname: page-component-78c5997874-4rdpn Total loading time: 0 Render date: 2024-11-02T18:46:20.737Z Has data issue: false hasContentIssue false
  • English
  • Français

Supernova Remnants with Radio Jets

Published online by Cambridge University Press:  04 August 2017

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

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Two examples are given of probable radio jet/supernova remnant association, G332.4+0.1 and G315.8-0.0. In both cases the jet length is larger than the radius of the remnant's shell; the jet diameter is barely resolved, and is substantially less than the observed shell thickness. The jet luminosity is 5–10% that of the shell. The G332.4+0.1 jet termi nates in an extended plume whose luminosity is ∼50% that of the shell.

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