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Gravitational-wave observations of binary black hole (BBH) systems point toblack hole spin magnitudes being relatively low. These measurements appear intension with high spin measurements for high-mass X-ray binaries (HMXBs). Weuse grids of MESA simulations combined with the rapid population-synthesis codeCOSMIC to examine the origin of these two binary populations. It has beensuggested that Case-A mass transfer while both stars are on the main sequencecan form high-spin BHs in HMXBs. Assuming this formation channel, we show thatdepending on critical mass ratios for the stability of mass transfer, 48-100%of these Case-A HMXBs merge during the common-envelope phase and up to 42%result in binaries too wide to merge within a Hubble time. Both MESA and COSMICshow that high-spin HMXBs formed through Case-A mass transfer can only formmerging BBHs within a small parameter space where mass transfer can lead toenough orbital shrinkage to merge within a Hubble time. We find that only up to11% of these Case-A HMXBs result in BBH mergers, and at most 20% of BBH mergerscame from Case-A HMXBs. Therefore, it is not surprising that these two spindistributions are observed to be different.

Do high-spin high-mass X-ray binaries contribute to the population of merging binary black holes?