Abstract
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 show that this is because they are moving at high velocity from the galactic plane,suggesting that they were formed a few million years ago very close to the galactic plane, within the normal population-l regions. Many 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, although some asymmetry in the formation event associated with the neutron star magnetic field is indicated.
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© 1985 D. Reidel Publishing Company, Dordrecht, Holland
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Lyne, A.G. (1985). The Kinematics of Pulsars. In: Boland, W., van Woerden, H. (eds) Birth and Evolution of Massive Stars and Stellar Groups. Astrophysics and Space Science Library, vol 120. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5478-6_23
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DOI: https://doi.org/10.1007/978-94-009-5478-6_23
Publisher Name: Springer, Dordrecht
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