Abstract
Analysis of a sample of pulsar proper-motions leads to the conclusion that most pulsars were born in and released from binary systems.
A minority of pulsars belong to a class characterized by low velocities and low magnetic fields. These were significantly spun-up by accretion and released from the binary through a non-explosive disruption of the companion. The rest belong to the high velocity, high magnetic field class. Using relations between the speeds at present and those in the binary orbit prior to its disruption, we show that such binaries must have undergone a common envelope phase of stellar evolution. The limits obtained on the masses and separations of these binary systems conform closely with those from stellar-evolution theory.
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Radhakrishnan, V., Shukre, C.S. (1987). The Binary Origin of Pulsar Velocities. In: Pacini, F. (eds) High Energy Phenomena Around Collapsed Stars. NATO ASI Series, vol 195. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3823-6_14
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DOI: https://doi.org/10.1007/978-94-009-3823-6_14
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