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Optical Studies of Supernova Remnants in the Magellanic Clouds

Published online by Cambridge University Press:  04 August 2017

D. S. Mathewson ,
V. L. Ford ,
M. A. Dopita ,
I. R. Tuohy ,
K. S. Long  and
D. J. Helfand
D. S. Mathewson
Affiliation:
Mount Stromlo and Siding Spring Observatories
V. L. Ford
Affiliation:
Mount Stromlo and Siding Spring Observatories
M. A. Dopita
Affiliation:
Mount Stromlo and Siding Spring Observatories
I. R. Tuohy
Affiliation:
Mount Stromlo and Siding Spring Observatories
K. S. Long
Affiliation:
Columbia University
D. J. Helfand
Affiliation:
Columbia University

Extract

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Optical identifications of 32 X-ray sources in the Magellanic Clouds confirm that they are SNRs. They are separated into four classes: the evolved, the oxygen-rich, the Balmer-dominated and the Crab-like. High velocity HI emission is observed from an extended region near 0525–66.0. It is suggested that this is produced by a possible Type III supernova which occurred out of the plane of the LMC and on the far side of the disk. The cumulative number-diameter relation for the LMC SNRs shows that they have evolved much faster than expected from the Sedov theory. It is suggested that this apparent “free-expansion” up to quite large diameters is due to the gradual conversion of the kinetic energy of the ejecta into thermal energy as they overtake the decelerating blast wave.

Type
VI. Supernova Remnants in Other Galaxies
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 541 - 549
Copyright
Copyright © Reidel 1983 

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