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Observations of G320.4–1.2 and Speculations on Supernova Remnant Morphology

Published online by Cambridge University Press:  04 August 2017

R. N. Manchester  and
J. M. Durdin
R. N. Manchester
Affiliation:
Division of Radiophysics, CSIRO, Sydney, Australia
J. M. Durdin
Affiliation:
Molonglo Radio Observatory, Hoskinstown, N.S.W., Australia

Extract

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The galactic radio source G320.4–1.2 (MSH15–52) consists of several components, the most prominent of which is situated in the north-west quadrant and is associated with the Hα nebula RCW89. Caswell et al. (1981) mapped the source at 1.4 GHz with a resolution of 50″ arc and concluded that it was a single supernova remnant with all components having spectral index α ≈ −0.34. This SNR has become more significant with the recent discovery (Seward and Harnden, 1982) of an X-ray pulsar of period 150 ms at the position (1950) R.A. 15h09m59s.5, Dec. −58°56′57″ near the centre of the remnant and the detection of this pulsar at radio frequencies (Manchester et al., 1982). The pulsar has some similarities to the Crab pulsar in that its period derivative is extremely high and hence its characteristic age low, ∼1570 years, comparable to that of the Crab pulsar. Timing observations (Manchester and Durdin, unpublished) indicate that the pulsar is not a member of a binary system and hence that the pulsed X-ray emission is powered by rotational energy, as in the Crab pulsar.

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. 421 - 427
Copyright
Copyright © Reidel 1983 

References

Blandford, R.D., and Rees, M.J.: 1974, Mon. Not. R. Astron. Soc. 169, p. 395.Google Scholar
Caswell, J.L.: 1977, Proc. Astron. Soc. Aust. 2, p. 130.Google Scholar
Caswell, J.L., Milne, D.K., and Wellington, K.J.: 1981, Mon. Not. R. Astron. Soc. 195, p. 89.Google Scholar
Day, G.A., Caswell, J.L., and Cooke, D.J.: 1972, Aust. J. Phys. Astrophys. Suppl. No. 25, p. 1.Google Scholar
Hamilton, P.A., McCulloch, P.M., Manchester, R.N., Ables, J.G., and Komesaroff, M.M.: 1977, Nature 265, p. 224.CrossRefGoogle Scholar
Kristian, J., Visvanathan, N., Westphal, J.A., and Snellen, G.H.: 1970, Astrophys. J. 162, p. 475.Google Scholar
Manchester, R.N., Tuohy, I.R., and D'Amico, N.: 1982, Astrophys. J. (Lett.) 262 (in press).Google Scholar
Mills, B.Y.: 1981, Proc. Astron. Soc. Aust. 4, p. 156.Google Scholar
Milne, D.K.: 1968, Aust. J. Phys. 21, p. 201.Google Scholar
Milne, D.K.: 1970, Aust. J. Phys. 23, p. 325.Google Scholar
Ostriker, J.P., and Gunn, J.E.: 1971, Astrophys. J. (Lett.) 164, p. L95.CrossRefGoogle Scholar
Ruderman, M.A., and Sutherland, P.G.: 1975, Astrophys. J. 196, p. 51.Google Scholar
Seward, F.D., and Harnden, F.R.: 1982, Astrophys. J. (Lett.) 256, p. L45.CrossRefGoogle Scholar
Shaver, P.A.: 1969, Observatory 89, p. 227.Google Scholar
Stephenson, F.R., Clark, D.H., and Crawford, D.F.: 1977, Mon. Not. R. Astron. Soc. 180, p. 567.Google Scholar
Weiler, K.W., and Panagia, N.: 1980, Astron. Astrophys. 90, p. 269.Google Scholar
Wilson, A.S.: 1972, Mon. Not. R. Astron. Soc. 157, p. 229.Google Scholar