Helium abundance profiles near the core-envelope boundary of stripped primaries from a few selected binary models at Solar metallicity. The selected binary models are the same as the ones shown in the left panel of Fig. 9. Diamonds mark the point to which each donor was stripped in mass transfer. Solid lines are taken from donor structures just after the end of mass transfer. Dashed lines show the extension of He profiles taken from the structure from the onset of mass transfer. The figure illustrates that the more massive the primary (M₁), the more massive the envelope that remains after mass transfer. As a result, stripped stars from models with M₁ ≳ 17 M_⊙ primaries may retain some envelope layers from the plateau of He abundance, leading to cooler effective temperatures (see Fig. 9 and the associated text).