Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-27T07:54:05.601Z Has data issue: false hasContentIssue false
  • English
  • Français

Secular Changes in the Flux Density of PSR 0833-45

Published online by Cambridge University Press:  25 April 2016

W. B. McAdam
W. B. McAdam*
Affiliation:
School of Physics, University of Sydney
Get access Rights & Permissions [Opens in a new window]

Extract

The pulsar 0833-45 associated with the Vela supernova remnant has been known as a strong source with fairly constant pulse amplitude since its discovery (Large, Vaughan & Mills 1968) using the east-west arm of the Molonglo telescope. The pulse stability together with the short period of 89 ms allowed its integrated flux to be seen also as a 1.7 Jy point source with the pencil beam of the full Cross, and a more precise declination was obtained. Further observations in 1971/72 with a beat period integrator used on the fan beams of the north-south arm showed that the pulsed radiation had the same declination as the point source within 2 arcsec (Vaughan & McAdam 1973). Monitoring observations in 1975/76 gave an independent position, and the mean of all Molonglo (408 MHz), Fleurs (1415 MHz) and NRAO interferometer (2700 MHz) positions led to the optical detection of the pulsar (Goss et al. 1977). The point source, therefore, is reliably identified with the pulsar.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 4 , Issue 2 , 1981 , pp. 219 - 221
Copyright
Copyright © Astronomical Society of Australia 1981

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

Backer, D. C., Astrophys. J., 190, 667 (1974).CrossRefGoogle Scholar
Cole, T. W., Hesse, H. K., and Page, C. G., Nature, 225, 712 (1970).CrossRefGoogle Scholar
Goss, W. M., Manchester, R. N., McAdam, W. B., and Frater, R. H., Mon. Not. R. Astron. Soc., 179, 51P (1977).CrossRefGoogle Scholar
Helfand, D. J., Fowler, L. A., and Kuhlman, J. V., Astron. J., 82, 701 (1977).CrossRefGoogle Scholar
Large, M. I., Vaughan, A. E., and Mills, B. Y., Nature, 220, 340 (1968).CrossRefGoogle Scholar
McAdam, W. B., Proc. Astron. Soc. Aust., 3, 283 (1978).CrossRefGoogle Scholar
McAdam, W. B., Proc. Astron. Soc. Aust., 4, 70 (1980).CrossRefGoogle Scholar
Rankin, J. M., Payne, R. R., and Campbell, D. B., Astrophys. J., 193, L71 (1974).CrossRefGoogle Scholar
Vaughan, A. E., and McAdam, W. B., Nature Phys. Sci., 241, 138 (1973).CrossRefGoogle Scholar