Properties after CE evolution for the case of donor stars with a radiative envelope, with artificially high values of α_CE = 10, 20 in order to allow for a successful CE ejection. Simulations correspond to binary systems composed of a star with a ZAMS mass of 30 M_⊙ and a BH companion of 3 M_⊙, with periods ranging from 10¹ days to 10³ days. Results are shown as a function of the radius of the star when it fills its Roche lobe. Top panel: central helium mass fraction Y_c at the onset of CE, showing RLOF before and after the end of the HG as a large drop in Y_c. Second panel: surface hydrogen mass fraction after envelope ejection. Third panel: stellar mass after envelope ejection, also showing the mass of the helium core defined as the innermost mass coordinate with Y > 0.01. Bottom panel: binding energy of the ejected envelope, as well as the binding energy that would be predicted by the Claeys et al. (2014) and Xu & Li (2010) fits, and the one corresponding to λ = 1.