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tokens: LIGO-Virgo network (1200 yr −1 detections at design sensitivity) under this model variation of Mandel de Mink ( 2016 ) and de Mink Mandel ( 2016 ). 6. Summary and Conclusion We have created and analyzed models of thermal winds from twin-star close binaries in circular orbits. Each of our models adopts q = 1, and we set the binary components surface based on a factor times the potential at the L 1 Lagrange point, f Φ . The wind initial sound speed is set based on a hydrodynamic escape parameter, λ . We examine the emergent wind distributions in each model, as well as the fluxes of mass and angular momentum carried away from the binary by the wind. Some key findings of our study are: 1. The acceleration of winds from about the binary components leads to a symmetric outflow traced by spiral density waves in the plane of the orbit (Figure 1 ). The subsonic acceleration region can surround either the individual binary components, or the entire binary, when f Φ ≲ λ /2 (Figure 2 ). The resulting outflow is largely similar to that of a spherical wind, with the addition of density and velocity waves in the equatorial plane due to the binary’s motion (Figure 1 ). 2. Eventual wind radial velocities are related to the surface sound speeds. At low sound speeds, radial velocities exceed that of a single-object wind model, implying that orbital motion imparts additional kinetic energy to the wind (Figures 3 and 4 ). 3. Mass loss rates from the binary are enhanced relative to the estimated superposition of two single-object winds. This effect is best modeled as a function of wind velocity, as shown in Figure 5 , and approximated by Equation ( 29 ). 4. The specific angular momentum carried by the wind depends primarily on the wind velocity as well (Figure 7 ). It is enhanced well beyond the binary’s specific angular momentum for the slower winds, which circulate around the binary before escaping near the outer Lagrange points (Figure 8 ), and we provide an approximating formula in Equation ( 32 ). The dependence of wind mass loss rate and specific angular momentum on wind velocity, as modeled by Equations ( 29 ) and ( 32 ) may have implications for models of massive, near-contact twin binaries undergoing chemically homogeneous evolution due to rotationally enhanced mixing. In particular, Mandel de Mink ( 2016 ) and de Mink Mandel ( 2016 ) argue that the model is sensitive to both the mass and angular momentum carried by winds. Our results suggest that for contact systems with low-velocity winds, mass loss rates and angular momentum loss rates will both be enhanced. Comparison to the model variations of Mandel de Mink ( 2016 ) and de Mink Mandel ( 2016 ) suggest that the high angular momentum loss rates may indicate an enhancement in the portion of binaries that undergo chemically homogeneous evolution that leave binary black hole remnants that can merge in a Hubble time. Productive avenues for future study include modeling twin-star winds that are radiatively,