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The Kinematics of Pulsars

Published online by Cambridge University Press:  04 August 2017

A.G. Lyne
A.G. Lyne*
Affiliation:
University of Manchester, Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire SK11 9DL, United Kingdom

Abstract

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Pulsars have a galactic radial distribution similar to that of many galactic populations such as HII regions, massive stars and supernova remnants. However they are generally much further from the plane of the Galaxy than these objects. Proper motion measurements sho that this is because they are typically moving with high velocities. The measurements also indicate that most pulsars were formed a few million years ago close to the plane, within the normal Population I regions. Some pulsars will escape from the Galaxy, although the majority will end up in a halo population. The origin of the high velocities is not clear at present but may be due either to some asymme try in the formation event or to the disruption of a close binary system.

Type
I. Rotation-Powered Pulsars
Information
Symposium - International Astronomical Union , Volume 125: The Origin and Evolution of Neutron Stars , 1987 , pp. 23 - 33
Copyright
Copyright © Reidel 1987 

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