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We use an analytic framework to calculate the evolution of binary orbitsunder a physically-motivated model that accounts for angular momentum lossassociated with winds from an accretion disk around the compact objectedaccretor. Our prescription considers wind mass ejection from the surface of anaccretion disk, accounting for a radial mass-loss dependence across the disksurface. We compare this to the standard prescription of angular momentum lossassociated with isotropic mass loss from the vicinity of the accretor. Theangular momentum loss from a disk-wind is always larger. For mass ratios, $q$,between $2$--$10$, angular momentum loss via a disk wind is $\simeq3$--$40$times greater than the standard prescription. For the majority of mass ratiosand disk properties, accounting for the disk wind can result in considerablysmaller orbital separations compared to the standard formalism; the differencesbeing $\simeq 60\%$ depending on how long the effect is integrated for. Weconclude that it is important to consider the effects of angular momentum lossfrom a disk wind when evolving binary orbits.

Angular Momentum Loss During Stable Mass Transfer onto a Compact object: the Effect of Mass Loss via Accretion Disk Winds