  We use an analytic framework to calculate the evolution of binary orbits
under a physically-motivated model that accounts for angular momentum loss
associated with winds from an accretion disk around the compact objected
accretor. Our prescription considers wind mass ejection from the surface of an
accretion disk, accounting for a radial mass-loss dependence across the disk
surface. We compare this to the standard prescription of angular momentum loss
associated with isotropic mass loss from the vicinity of the accretor. The
angular 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 ratios
and disk properties, accounting for the disk wind can result in considerably
smaller orbital separations compared to the standard formalism; the differences
being $\simeq 60\%$ depending on how long the effect is integrated for. We
conclude that it is important to consider the effects of angular momentum loss
from a disk wind when evolving binary orbits.
