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High mass X-ray binaries as progenitors of gravitational wave sources

Published online by Cambridge University Press:  30 December 2019

Jakub Klencki Open the ORCID record for Jakub Klencki [Opens in a new window]  and
Gijs Nelemans
Jakub Klencki
Affiliation:
Department of Astrophysics/IMAPP, Radboud University, P O Box 9010, NL-6500 GL Nijmegen, The Netherlands emails: j.klencki@astro.ru.nl, nelemans@astro.ru.nl
Gijs Nelemans
Affiliation:
Department of Astrophysics/IMAPP, Radboud University, P O Box 9010, NL-6500 GL Nijmegen, The Netherlands emails: j.klencki@astro.ru.nl, nelemans@astro.ru.nl Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
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Abstract

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X-ray binaries with black hole (BH) accretors and massive star donors at short orbital periods of a few days can evolve into close binary BH (BBH) systems that merge within the Hubble time. From an observational point of view, upon the Roche-lobe overflow such systems will most likely appear as ultra-luminous X-ray sources (ULXs). To study this connection, we compute the mass transfer phase in systems with BH accretors and massive star donors (M > 15 Mʘ) at various orbital separations and metallicities. In the case of core-hydrogen and core-helium burning donors (cases A and C of mass transfer) we find the typical duration of super-Eddington mass transfer of up to 106 and 105 yr, with rates of 10−6 and 10−5Mʘ yr-1, respectively. Given that roughly 0.5 ULXs are found per unit of star formation rate, we estimate the rate of BBH mergers from stable mass transfer evolution to be at most 10 Gpc−3 yr−1.

Keywords

X-rays: binaries(stars:) binaries (including multiple): closestars: evolution
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. 417 - 425
Copyright
© International Astronomical Union 2019 

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