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Origin of pulsars with 0.1 s < P < 0.3 s and 5 × 105 years <  < 107 years after the second supernova explosion in high-mass X-ray binaries

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The origin of same of the single pulsars with relatively low magnetic fields B < 1012 G and with characteristic times  < 107 years is established. Such pulsars occur as a result of the disruption of high-mass X-ray binary systems after a second supernova explosion. In these binaries, mass accretion on to the surface of X-ray pulsars leads to the decrease in the magnetic field from its initial value B ≈ 1012-1013 G down to B < 1012 G similar to the processes in low mass X-ray binaries.

Keywords: Evolution; Origin; Pulsars

Document Type: Research Article


Affiliations: 1: Department of Physics Middle East Technical University Ankara 06531 Turkey 2: Academy of Science Physics Institute Baku 370143 Azerbaijan

Publication date: August 1, 2004

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