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Be X-ray binaries in the SMC as indicators of mass transfer efficiency
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Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star companions accreting from the circumstellar emission disk. We compare the observed population of BeXRBs in the Small Magellanic Cloud with simulated populations of BeXRB-like systems produced with the COMPAS population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXRBs than in the Be population at large. Assuming that BeXRBs experienced only dynamically stable mass transfer, their mass distribution suggests that at least 30% of the mass donated by the progenitor of the neutron star is typically accreted by the B-star companion. We expect these results to affect predictions for the population of double compact object mergers. A convolution of the simulated BeXRB population with the star formation history of the Small Magellanic Cloud shows that the excess of BeXRBs is most likely explained by this galaxy's burst of star formation around 20--40 Myr ago.
Forward citations
Cited by 2 Pith papers
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Stable mass transfer in massive binaries leading to merging black holes
Stable mass transfer in massive binaries, modeled with the accreting star's altered structure, produces merging black holes matching LIGO/Virgo masses and spins.
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X-Ray Views of Galactic Accreting Pulsars in High-Mass X-Ray Binaries
A concise review of the timing, spectral, and polarization properties of accreting X-ray pulsars in high-mass X-ray binaries, including recent IXPE results.
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