Birth kicks as the origin of pulsar rotation

H. Spruit () and E. S. Phinney
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H. Spruit: Max-Planck-Institut für Astrophysik
E. S. Phinney: European Southern Observatory

Nature, 1998, vol. 393, issue 6681, 139-141

Abstract: Abstract Radio pulsars are thought to born with spin periods of 0.02–0.5 s and space velocities of 100–1,000 km s−1, and they are inferred to have initial dipole magnetic fields of 1011–1013 G (1–5). The average space velocity of their progenitor stars is less than 15 km s−1, which means that pulsars must receive a substantial ‘kick’ at birth. Here we propose that the birth characteristics of pulsars have a simple physical connection with each other. Magnetic fields maintained by differential rotation between the core and envelope of the progenitor would keep the whole star in a state of approximately uniform rotation until10 years before the explosion. Such a slowly rotating core has 1,000 times less angular momentum than required to explain the rotation of pulsars. The specific physical process that ‘kicks’ the neutron star at birth has not been identified, but unless its force is exerted exactly head-on6 it will also cause the neutron star to rotate. We identify this process as the origin of the spin of pulsars. Such kicks may cause a correlation between the velocity and spin vectors of pulsars. We predict that many neutron stars are born with periods longer than 2 s, and never become radio pulsars.

Date: 1998
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DOI: 10.1038/30168

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