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Evolution of the Radio Remnant of SN 1987A: 1990-2001

Published online by Cambridge University Press:  05 March 2013

R. N. Manchester ,
B. M. Gaensler ,
V. C. Wheaton ,
L. Staveley-Smith ,
A. K. Tzioumis ,
N. S. Bizunok ,
M. J. Kesteven  and
J. E. Reynolds
R. N. Manchester*
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710
B. M. Gaensler
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710
V. C. Wheaton
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710 School of Physics, University of Sydney, NSW 2006
L. Staveley-Smith
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710
A. K. Tzioumis
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710
N. S. Bizunok
Affiliation:
Center for Space Research, Massachusetts Institute of Technology, Cambridge MA 02139, USA Boston University, Boston MA 02215, USA
M. J. Kesteven
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710
J. E. Reynolds
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710
*
[email protected]
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Abstract

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The development of the radio remnant of SN 1987A has been followed using the Australia Telescope Compact Array since its first detection in 1990 August. The remnant has been observed at four frequencies, 1.4, 2.4, 4.8, and 8.6 GHz, at intervals of 4–6 weeks since the first detection. These data are combined with the 843 MHz data set of Ball et al. (2001) obtained at Molonglo Observatory to study the spectral and temporal variations of the emission. These observations show that the remnant continues to increase in brightness, with a larger rate of increase at recent times. They also show that the radio spectrum is becoming flatter, with the spectral index changing from −0.97 to −0.88 over the 11 years. In addition, at roughly yearly intervals since 1992, the remnant has been imaged at 9 GHz using super-resolution techniques to obtain an effective synthesised beamwidth of about 0″.5. The imaging observations confirm the shell morphology of the radio remnant and show that it continues to expand at ˜3000 km s−1. The bright regions of radio emission seen on the limb of the shell do not appear to be related to the optical hot spots which have subsequently appeared in surrounding circumstellar material.

Keywords

circumstellar matterradio continuum: ISMsupernovae: individual (SN 1987A)supernova remnants
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 19 , Issue 2 , 2002 , pp. 207 - 221
Copyright
Copyright © Astronomical Society of Australia 2002

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