Change in the semilatus rectum of the inner orbit () between the ZAMS and the onset of mass transfer. The figure shows the cumulative distribution of the logarithm of 𝒜 = a_p, init/a_p, final for model OBin, while other models show qualitatively similar behaviour. LK cycles with tidal friction drive the inner stars closer together (𝒜 >  1), whereas stellar winds act to widen the orbit (𝒜 <  1). The figure shows that LKCTF can shrink the inner orbit most efficiently for low-mass MS stars, followed by higher-mass MS stars, and evolved stars.