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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 

References

Blair, W.P., Kirshner, R.P. and Chevalier, R.A.: 1981, Astrophys. J., 247, 879.CrossRefGoogle Scholar
Clark, D.H., Tuohy, I.R., Long, K.S., Szymkowiak, A.E., Dopita, M.A., Mathewson, D.S., and Culhane, J.H.: 1982, Astrophys. J., 255, 440.Google Scholar
Danziger, I.J. and Dennefeld, M.: 1976, Astrophys. J., 207, 394.Google Scholar
Danziger, I.J., Goss, W.M., Murdin, P., Clark, D.H., and Boksenberg, A.: 1981, Monthly Notices Roy. Astron. Soc., 195, 33P.Google Scholar
Davies, R.D., Elliott, K.H., and Meaburn, J.: 1976, Memoirs of the Roy. Astron. Soc., 81, 89.Google Scholar
Dopita, M.A.: 1979, Astrophys. J. Suppl., 40, 455.Google Scholar
Dopita, M.A., Tuohy, I.R., and Mathewson, D.S.: 1981, Astrophys. J. (Letters), 248, L105.CrossRefGoogle Scholar
Gorenstein, P., Seward, F., and Tucker, W.: 1983, this volume, p. 1.Google Scholar
Gull, T.R. and Fesen, R.A.: 1982, Astrophys. J. (Letters), 260, L75.Google Scholar
Henize, K.G.: 1956, Astrophys. J. Suppl., 2, 315.Google Scholar
Lasker, B.M.: 1980, Astrophys. J., 237, 765.CrossRefGoogle Scholar
Long, K.S., Helfand, D.J., and Grabelsky, D.A.: 1981, Astrophys. J., 248, 925.CrossRefGoogle Scholar
McKee, C.F. and Ostriker, J.P.: 1977, Astrophys. J., 218, 148.CrossRefGoogle Scholar
Mathewson, D.S. and Clarke, J.N.: 1973, Astrophys. J., 179, 89.CrossRefGoogle Scholar
Mathewson, D.S., Dopita, M.A., Tuohy, I.R., and Ford, V.L.: 1980, Astrophys. J. (Letters), 242, L73.CrossRefGoogle Scholar
Mathewson, D.S., Ford, V.L., Dopita, M.A., Tuohy, I.R., Long, K.S., and Helfand, D.J.: 1983, Astrophys. J. Suppl., in press.Google Scholar
Mills, B.Y., Little, A.G., Durdin, J.M., and Kesteven, M.J.: 1982, Monthly Notices Roy. Astron. Soc., 200, 1007.CrossRefGoogle Scholar
Seward, F.D. and Mitchell, M.: 1981, Astrophys. J., 243, 736.Google Scholar
Tanaka, Y.: 1983, these proceedings.Google Scholar
Tuohy, I.R., Dopita, M.A., Mathewson, D.S., Long, K.S., and Helfand, D.J.: 1983, this volume, p. 571.Google Scholar
Weiler, K.W.: 1983, this volume, p. 299.Google Scholar