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We explore the consequences of dynamical evolution of field binaries composedof a primary black hole (BH) and a Wolf-Rayet (WR) star in the context ofgravitational wave (GW) source progenitors. We argue, from generalconsiderations, that the spin of the WR-descendent BH will be maximal in asignificant number of cases due to dynamical effects. In other cases, the spinshould reflect the natal spin of the primary BH which are currentlytheoretically unconstrained. We argue that the three currently published LIGOsystems (GW150914, GW151226, LVT151012) suggest that this spin is small. Theresultant effective spin distribution of gravitational wave sources should thusbe bi-model if this classic GW progenitor channel is indeed dominant. Whilethis is consistent with the LIGO detections thus far, it is in contrast to thethree best-measured high-mass x-ray binary (HMXB) systems. A comparison of thespin distribution of HMXBs and GW sources should ultimately reveal whether ornot these systems arise from similar astrophysical channels.

Research Note: The Expected Spins of Gravitational Wave Sources With Isolated Field Binary Progenitors