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High-Mass X-ray Binaries: progenitors of double compact objects

Published online by Cambridge University Press:  30 December 2019

Edward P. J. van den Heuvel
Edward P. J. van den Heuvel*
Affiliation:
Anton Pannekoek Institute of Astronomy, University of Amsterdam, Postbus 92429, NL-1090GE, Amsterdam, the Netherlands email: E.P.J.vandenHeuvel@uva.nl
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Abstract

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A summary is given of the present state of our knowledge of High-Mass X-ray Binaries (HMXBs), their formation and expected future evolution. Among the HMXB-systems that contain neutron stars, only those that have orbital periods upwards of one year will survive the Common-Envelope (CE) evolution that follows the HMXB phase. These systems may produce close double neutron stars with eccentric orbits. The HMXBs that contain black holes do not necessarily evolve into a CE phase. Systems with relatively short orbital periods will evolve by stable Roche-lobe overflow to short-period Wolf-Rayet (WR) X-ray binaries containing a black hole. Two other ways for the formation of WR X-ray binaries with black holes are identified: CE-evolution of wide HMXBs and homogeneous evolution of very close systems. In all three cases, the final product of the WR X-ray binary will be a double black hole or a black hole neutron star binary.

Keywords

Common Envelope Evolutionneutron starblack holedouble neutron stardouble black holeWolf-Rayet X-ray Binaryformationevolution
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. 1 - 13
Copyright
© International Astronomical Union 2019 

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