Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-25T16:13:00.026Z Has data issue: false hasContentIssue false
  • English
  • Français

Millisecond Pulsar Surveys

Published online by Cambridge University Press:  12 April 2016

M. Bailes
M. Bailes*
Affiliation:
Physics Department, University of Melbourne, Parkville, Victoria 3052, Australia. email: [email protected]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

There are now more than 30 millisecond pulsars known to be associated with the Galactic disk. The majority of these have been discovered in just the last few years as the result of large-scale all-sky surveys. The properties of the population vary tremendously. One unique object hosts a planetary system, more than half of those discovered possess white dwarf companions, two have extremely low-mass companions that are undergoing mass-loss and several others appear to be solitary. In this review I discuss the methods employed to find these millisecond pulsars, the parallels with early surveys for “normal” pulsars, and possible strategies for future searches.

Type
Part 1 The Pulsar Population
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 3 - 10
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

Alpar, A. et al. 1982, Nature, 300, 728.CrossRefGoogle Scholar
Backer, D.C. et al. 1982, Nature, 300, 615.CrossRefGoogle Scholar
Bailes, M. & Johnston, S., 1993, in “Review of Radio Science 1990-1992”, ed Stone, W.R., Oxford University Press, p 677 Google Scholar
Bailes, et al., 1996, ApJ, in prep.Google Scholar
Camilo, F., Nice, D. & Taylor, J.H., 1993, ApJ, 412, L37.Google Scholar
Camilo, F. 1996, in “High Sensitivity Radio Astronomy”, Cambridge University Press.Google Scholar
Clifton, T.R., & Lyne, A.G., 1986, Nature, 320, 43.CrossRefGoogle Scholar
Curran, , & Lorimer, D.R., 1995, MNRAS, 276, 347.Google Scholar
Dewey, R.J. et al., 1984, in “Millisecond Pulsars”, eds Reynolds, S.P. & Stinebring, D.R., NRAO Green Bank, p. 234 Google Scholar
Foster, R.S., Cadwell, B.J., Wolszczan, A. & Anderson, S.B., 1995, ApJ, 454, 826.CrossRefGoogle Scholar
Fruchter, A.S., Stinebring, D.R. & Taylor, J.H., 1988, Nature, 333, 237.Google Scholar
Hulse, R.A. & Taylor, J.H., 1975, ApJ, 201 L55.Google Scholar
Johnston, S. & Bailes, M., 1991, MNRAS, 252, 277.Google Scholar
Johnston, et al. 1992, MNRAS, 255, 401.Google Scholar
Lorimer, et al. 1995, ApJ, 439, 933.Google Scholar
Lundgren, S.C., Zepka, A.F., & Cordes, J.M., 1995, ApJ, 453, 419.Google Scholar
Manchester, et al. 1996, MNRAS, 279, 1235.Google Scholar
Manchester, R.N. & Taylor, J.H., 1977, “Pulsars”, Freeman, San Francisco.Google Scholar
Navarro, J.N. et al., 1995, ApJ, 455, L55.Google Scholar
Nicastro, L. et al., 1995, MNRAS, 273, L68.Google Scholar
Nice, D., Taylor, J.H. & Fruchter, A.S., 1993, ApJ, 402, L49.Google Scholar
Phinney, E.S., 1991, ApJ, 380, L17.Google Scholar
Romani, R. 1989, in “Timing Neutron Stars”, Kluwer, eds Ögelman, & van den, Heuvel, p 113.Google Scholar
Ryba, M. & Taylor, J.H., 1991, ApJ, 371, 739.Google Scholar
Sayer, R.W., Nice, D.J. & Taylor, J.H., 1996, ApJ, submitted.Google Scholar
Segelstein, et al., 1986, Nature, 322, 714.Google Scholar
Stinebring, et al, 1990, Phys.Rev.Lett, 65, 285.Google Scholar
Weisberg, & Taylor, J.H., 1984, Phys. Rev. L., 52, 1348.Google Scholar
Wolszczan, A., 1990, IAU circular 5073.Google Scholar