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The Ellery Lecture 1993: Pulsars—Setting the Standard

Published online by Cambridge University Press:  25 April 2016

R. N. Manchester
R. N. Manchester*
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 2121
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Abstract

Over 600 pulsars are now known, almost all of which lie in our Galaxy. Most pulsars have periods between 0 · 1 and a few seconds, but a very important sub-class, the ‘millisecond’ pulsars, have much shorter periods. Millisecond pulsars are often in a binary orbit with another star, suggesting that their short periods are a result of accreting mass from the companion star. They are also extraordinarily good clocks, with a stability comparable to that of the best atomic clocks. This combination of extreme period stability and binary motion has led to some very important results, including the first observational evidence for gravitational radiation and the first evidence for extra-solar planetary systems. It is probable that pulsars will be used to define the long-term standard of terrestrial time. A search of the southern sky using the Parkes radio telescope has found several millisecond pulsars which will make an important contribution to these precision-timing programs.

Type
Invited
Information
Publications of the Astronomical Society of Australia , Volume 11 , Issue 1 , April 1994 , pp. 1 - 6
Copyright
Copyright © Astronomical Society of Australia 1994

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References

Backer, D.C. and Hellings, R. W., 1986, ARA&A, 24, 537.Google Scholar
Backer, D.C., Kulkami, S. R., Heiles, C., Davis, M. M. and Goss, W. M., 1982, Nature, 300, 615.Google Scholar
Bailes, M., et al. 1994, ApJ, in press.Google Scholar
Bell, J. F., Bailes, M. and Bessel, M. F., 1993, Nature, 364, 603.CrossRefGoogle Scholar
Bhattacharya, D. and van den Heuvel, E. P. J., 1991, Phys. Reports, 203, 1.Google Scholar
Blandford, R. D., Romani, R. W. and Applegate, J. H., 1987, MNRAS, 225, 51P.Google Scholar
Cordes, J. M. and Downs, G. S., 1985, ApJS, 59, 343.Google Scholar
Damour, T. and Taylor, J. H., 1992, Phys. Rev. D 45, 1840.Google Scholar
Foster, R. S. and Backer, D. C., 1990, ApJ, 361, 300.Google Scholar
Gold, T., 1968, Nature, 218, 731.Google Scholar
Hewish, A., Bell, S. J., Pilkington, J. D. H., Scott, P. F. and Collins, R. A., 1968, Nature, 217, 709.Google Scholar
Hut, P., Murphy, B. W. and Verbunt, F., 1991, A&A, 241, 137.Google Scholar
Johnston, S., et al, 1993, Nature, 361, 613.CrossRefGoogle Scholar
Kaspi, V. M., Taylor, J. H. and Ryba, M., 1994, ApJ, in press.Google Scholar
Kulkarni, S. R., 1986, ApJ, 306, L85.CrossRefGoogle Scholar
Manchester, R. N., Lyne, A. G., Robinson, C., D’Amico, N. D., Bailes, M. and Lim, J., 1991, Nature, 352, 219.Google Scholar
McCulloch, P. M., Hamilton, P. A., McConnell, D., and Kin, E. A., 1990, Nature, 346, 822.CrossRefGoogle Scholar
Phinney, E. S., 1992, Phil. Trans. Roy. Soc., A 341, 39.Google Scholar
Taylor, J. H., and Weisberg, J. M., 1989, ApJ, 345, 434.Google Scholar
Taylor, J. H., Wolszczan, A., Damour, T. and Weisberg, J.M., 1992, Nature, 355, 132.Google Scholar
Taylor, J. H., Manchester, R. N. and Lyne, A. G., 1993, ApJS, 88, 529.Google Scholar
Wolszczan, A. and Frail, D. A., 1992, Nature, 355, 145.CrossRefGoogle Scholar