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Supernova Remnants with Central Pulsars

Published online by Cambridge University Press:  04 August 2017

Frederick D. Seward
Frederick D. Seward*
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass. Institute of Astronomy, Cambridge, England

Abstract

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The recent discovery of a central pulsing X-ray source makes MSH 15–52 the third SNR to contain a radio pulsar surrounded by diffuse X-ray emission. The pulsar periods are all increasing with time and the consequent loss of rotational kinetic energy is enough, in each remnant, to power a synchrotron nebula with the observed luminosity and volume.

After a review of the properties of the Crab Nebula it will be shown that both Vela X and MSH 15–52 have the same relationship between central pulsar and diffuse emission. Using empirical rules derived from these SNR, it is demonstrated that other plerionic remnants have similar characteristics. Two accretion-powered central sources can be distinguished from radio pulsars in SNR by the relatively high X-ray luminosity of the central source compared to that of possible synchrotron diffuse emission.

Type
V. Compact Objects Associated With Supernova Remnants, Pulsars and Neutron Stars
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 405 - 416
Copyright
Copyright © Reidel 1983 

References

Becker, R. & Szymkowiak, A. (1981) Ap. J. Letters, 248, L23.Google Scholar
Becker, R., Helfand, D. & Szymkowiak, A. (1982) Ap. J., 255, 557.Google Scholar
Bignami, G.F. & Hermsen, W. (1982) Ann. Rev. Ast. Ap. 21 in press.Google Scholar
Caswell, J.L. (1979) MN 187, 431.Google Scholar
Caswell, J.L., Milne, D.K. & Wellington, K.J. (1981) MN 195, 89.Google Scholar
Chiappetti, L. & Bell-Burnell, S.J. (1982) MN in press.Google Scholar
Crampton, D., Cowley, A. & Hutchings, J. (1980) Ap. J. Letters 235, L131.Google Scholar
Davies, R.D. & Smith, F.G. ed. (1971) “The Crab Nebula” IAU Symposium 46.Google Scholar
Gregory, P. (1983), this volume, p. 441.Google Scholar
Harnden, F.R. Jr. (1983), this volume, p. 131.Google Scholar
Helfand, D. (1981) IAU Symposium 95, 343.CrossRefGoogle Scholar
Helfand, D. (1983), this volume, p. 483.Google Scholar
Hjelming, R.M. & Wade, C.M. (1971) Ap. J. Letters 164, L1.CrossRefGoogle Scholar
Lamb, R.C. & Markert, T.H. (1981) Ap. J. 244, 94.Google Scholar
Lockhart, J.A., Goss, W.M., Caswell, J.L. & McAdam, W.B. (1977) MN 179, 147.Google Scholar
Manchester, R.N. & Taylor, J.H. (1977) “Pulsars” W.H. Freeman & Co.Google Scholar
Manchester, R.N., Tuohy, I. & D'Amico, N. (1982) Ap. J. Letters in press.Google Scholar
Pravdo, S.H., Becker, R.H., Boldt, E.A., Holt, S.S., Serlemitsos, P.J. & Swank, J.H. (1978) Ap. J. 223, 537.CrossRefGoogle Scholar
Seward, F.D. & Harnden, F.R. Jr. (1982) Ap. J. Letters 256, L45.Google Scholar
Seward, F.D., Harnden, F.R. Jr., Murden, P. & Clark, D.H. (1982) submitted to Ap. J. Google Scholar
Smith, A. (1978) MN 182, 39P.Google Scholar
Toor, A. & Seward, F.D. (1974) Ast. J. 79, 995.CrossRefGoogle Scholar
Tuohy, I. & Garmire, G. (1980) Ap. J. Letters 239, L107.CrossRefGoogle Scholar
Watson, M.G., Willingale, R., Grindlay, J.E., Seward, F.D. (1982) in preparation.Google Scholar
Weiler, K.W. & Shaver, P.A. (1978) Astron. & Ap. 70, 389.Google Scholar
Wilson, A.S. (1980) Ap. J. Letters 241, L19.CrossRefGoogle Scholar