English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutronstar companions accreting from the circumstellar emission disk. We compare theobserved population of BeXRBs in the Small Magellanic Cloud with simulatedpopulations of BeXRB-like systems produced with the COMPAS population synthesiscode. We focus on the apparently higher minimal mass of Be stars in BeXRBs thanin the Be population at large. Assuming that BeXRBs experienced onlydynamically stable mass transfer, their mass distribution suggests that atleast 30% of the mass donated by the progenitor of the neutron star istypically accreted by the B-star companion. We expect these results to affectpredictions for the population of double compact object mergers. A convolutionof the simulated BeXRB population with the star formation history of the SmallMagellanic Cloud shows that the excess of BeXRBs is most likely explained bythis galaxy's burst of star formation around 20--40 Myr ago.

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