Hostname: page-component-848d4c4894-wzw2p Total loading time: 0 Render date: 2024-05-09T15:35:14.009Z Has data issue: false hasContentIssue false
  • English
  • Français

The velocity distribution of young radio pulsars: simulating the observations

Published online by Cambridge University Press:  12 April 2016

J.W. Hartman
J.W. Hartman*
Affiliation:
Astronomical Institute, Utrecht, the Netherlands

Extract

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.

Lyne & Lorimer (1994) argue that the velocities of young pulsars are much higher than was previously thought. However, recent radio pulsar population synthesis work by Hartman et al. (1996, these proceedings) shows that simulations that use a birth velocity distribution with more pulsars at low velocities, Phinney’s modification of the Paczyński (1990) distribution

describes the observed magnetic field, period and luminosity distribution equally well as simulations that use the Lyne & Lorimer distribution.

We use this radio pulsar population synthesis model to obtain the proper motion distribution of the simulated sample, and from that we calculate the transverse velocity distribution to compare it with the observed transverse velocity distribution. A full report of this work will be given in Hartman (1996).

Type
Part 1 The Pulsar Population
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 53 - 54
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

Bhattacharya, D., Wijers, R., Hartman, J., Verbunt, F. 1992, A&A, 254, 198 Google Scholar
Hartman, J., 1996, A&A in prep.Google Scholar
Lyne, A., Lorimer, D. 1994, Nat, 369, 127 Google Scholar
Paczyński, B. 1990, ApJ, 348, 485 Google Scholar
Taylor, J., Manchester, R., Lyne, A. 1993, ApJS, 88, 529 Google Scholar