Hostname: page-component-848d4c4894-xm8r8 Total loading time: 0 Render date: 2024-06-14T03:38:18.506Z Has data issue: false hasContentIssue false
  • English
  • Français

Supernova Remnants, Pulsars and X-Ray Sources

Published online by Cambridge University Press:  25 April 2016

D. K. Milne
D. K. Milne*
Affiliation:
Division of Radiophysics, CSIRO, Sydney
Get access Rights & Permissions [Opens in a new window]

Extract

From an assessment of recent high-resolution galactic radio surveys, in the continuum and in the H109oc recombination line, the author has detected or confirmed over 90 non-thermal sources, most likely all supernova remnants.1 The distances to each of these objects have also been estimated, from an empirical surface-brightness linear-size relationship derived from 15 remnants whose distances are known from either a comparison of the radial velocities and proper motions of filaments in the nebula, neutral hydrogen absorption measurements, or association of the remnant with an object of known distance. In this note we wish to remark on the galactic distribution of supernova remnants and the possible association of these objects with pulsars and X-ray sources.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 1 , Issue 7 , April 1970 , pp. 333 - 334
Copyright
Copyright © Astronomical Society of Australia 1970

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

1 Milne, D. K., Aust. J. Phys., in press.Google Scholar
2 Kerr, F. J. and Westerhout, G., In ‘Stars and Stellar Systems’. Vol. V, eds, Blaauw, A. and Schmidt, M., University of Chicago Press, Chicago 1965, pp. 167–202.Google Scholar
3 McGee, R. X., Gardner, F. F. and Robinson, B. J., Aust. J. Phys., 20, 407 (1967).CrossRefGoogle Scholar
4 Wilson, T. L., Mezger, P. G., Gardner, F. F. and Milne, D. K., in preparation, 1969.Google Scholar
5 Radhakrishnan, V., Proc. ASA, 1, 254 (1969).Google Scholar
6 Large, M. I., Vaughan, A. E. and Wielebinski, R., Nature, 223, 1249 (1969).Google Scholar
7 Staelin, D. H. and Reifenstein, E. C., Ap. J., 156, L121 (1969).Google Scholar
8 Large, M. I., Vaughan, A. E. and Mills, B. Y., Nature, 220, 340 (1968).CrossRefGoogle Scholar
9 Reifenstein, E. C., Brundage, W. D. and Staelin, D. H., Ap. J., 156, L125 (1969).Google Scholar
10 Large, M. I., Astrophys. Lett. 5, 11 (1970).Google Scholar
11 Webber, W. R., Proc. ASA, 1, 160 (1968).Google Scholar
12 Lewin, W. H. G., Clark, G. W. and Smith, W. B., Ap. J., 152, L49 (1968).Google Scholar
13 Bradt, H., Naranan, S., Rappaport, S. and Spada, G., Ap. J., 152, 1005 (1968).Google Scholar
14 Eggen, O. J., Freeman, K. C. and Sandage, A., Ap. J., 154, L27 (1968).Google Scholar
15 Fisher, P. C., Jordan, W. C., Meyerott, A. J., Acton, L. W. and Roethig, D. T., Ap. J., 151, 1 (1968).Google Scholar
16 Milne, D. K., Nature, 224, 891 (1969).Google Scholar