Be X-ray binaries in the SMC as indicators of mass-transfer efficiency

Serena Vinciguerra, Coenraad J. Neijssel, Alejandro Vigna-Gómez, Ilya Mandel, Philipp Podsiadlowski, Thomas J. Maccarone, Matt Nicholl, Samuel Kingdon, Alice Perry, Francesco Salemi

Research output: Contribution to journalArticlepeer-review

1 Scopus citations

Abstract

Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star (NS) companions accreting from the circumstellar emission disc. We compare the observed population of BeXRBs in the Small Magellanic Cloud (SMC) 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 per cent of the mass donated by the progenitor of the NS 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 SMC shows that the excess of BeXRBs is most likely explained by this galaxy's burst of star formation ∼20-40 Myr ago.

Original languageEnglish
Pages (from-to)4705-4720
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume498
Issue number4
DOIs
StatePublished - Nov 1 2020

Keywords

  • Be
  • Gravitational waves
  • Methods: data analysis
  • Stars: emission-line
  • Stars: evolution
  • Stars: neutron
  • X-rays: binaries

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