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Structure in the Radio Remnant of Supernova 1987A

Published online by Cambridge University Press:  25 April 2016

L. Staveley-Smith ,
R.N. Manchester ,
M.J. Kesteven ,
A.K. Tzioumis  and
J.E.R. Reynolds
L. Staveley-Smith
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 2121
R.N. Manchester
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 2121
M.J. Kesteven
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 2121
A.K. Tzioumis
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 2121
J.E.R. Reynolds
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 2121
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Abstract

The radio emission associated with SN 1987A appears to be synchrotron emission resulting from the acceleration of electrons at the interface between the outward moving shock wave and clumps of circumstellar material. The Australia Telescope Compact Array is now able to resolve this region, which has dimensions of ~ arcsec, revealing a slight (10%) asphericity in the distribution of the low density gas within the [OIII] circumstellar ring. Assuming that the radio emission arises from a region just behind the shock front, we deduce a mean radial expansion velocity, from 1987 to 1992, of 29 200 kms. First observed contact of the shock with the [OIII] circumstellar ring could occur as early as mid-1993, depending on the deceleration in the intervening gas. This will probably be closely followed by shock-excited optical lines, a strong X-ray outburst and a further increase in the radio emission.

Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 4 , 1993 , pp. 331 - 334
Copyright
Copyright © Astronomical Society of Australia 1993

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