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SN 1987A at Radio Wavelengths

Published online by Cambridge University Press:  19 September 2016

L. Staveley-Smith ,
R.N. Manchester ,
B.M. Gaensler ,
M.J. Kesteven ,
A.K. Tzioumis ,
N.S. Bizunok  and
V.C. Wheaton
L. Staveley-Smith
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia;[email protected]
R.N. Manchester
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia;[email protected]
B.M. Gaensler
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St. MS-6, Cambridge, MA 02138, USA
M.J. Kesteven
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia;[email protected]
A.K. Tzioumis
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia;[email protected]
N.S. Bizunok
Affiliation:
Boston University, Boston, MA 02215, USA
V.C. Wheaton
Affiliation:
School of Physics, University of Sydney, NSW 2006, Australia

Summary

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SN1987A has an intrinsic radio luminosity some four orders of magnitude less than SN1993J at maximum, largely a reflection of the tenuous wind . from the progenitor of SN1987A before explosion. Both remnants have an edge-brightened, ring-like morphology though, in the case of SN1987A, the expansion rate is currently only around 3500 km s−1. The flux density of the remnant of SN1987A continues to rise at all measured radio frequencies. Its spectral index is gradually flattening, indicating its transition into the supernova remnant phase. A campaign to increase the resolution of radio imaging by observing at higher frequencies is underway with the Australia Telescope Compact Array (ATCA).

Type
Part I Supernovae: Individual
Information
International Astronomical Union Colloquium , Volume 192: Cosmic Explosions , 2005 , pp. 89 - 95
Copyright
Copyright © Springer-Verlag 2005

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