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Evolution of High-mass X-ray binaries in the Small Magellanic Cloud

Published online by Cambridge University Press:  30 December 2019

Jun Yang  and
Daniel R. Wik
Jun Yang*
Affiliation:
Department of Physics and Astronomy, the University of Utah, Salt Lake City, Utah 84112, USA
*
email: [email protected]
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Abstract

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In order to understand the progenitor of rotation powered pulsars, we compare them with High-mass X-ray binary (HMXB) pulsars, (or X-ray pulsars), in the Small Magellanic Cloud. The plot of period period vs. period derivative shows that isolated neutron stars could be evolved from HMXBs. The pulsars with long spin period might spin up to 0.001-1 s. The mechanism is a third-body interaction that detaches the donor, leaving an isolated, small period neutron star behind.

Keywords

pulsars: generalstars: neutronstars: evolutionX-rays: binariesaccretionaccretion disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 353 - 357
Copyright
© International Astronomical Union 2019 

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