The relative standard deviation of the accretion rate onto the primary (﹩\delta {\dot{M}}_{1}﹩) and onto the secondary (﹩\delta {\dot{M}}_{2}﹩), computed over the final 500 orbital periods of each simulation. Accretion is never steady in an absolute sense. However, in cases where the cavity eccentricity is below e ≲ 10⁻³ or so, the level of normalized variability is below ∼1%. At most mass ratios, the degree of variability is greater for binaries in colder disks.