Notes. The types of stars correspond to the definition by Hurley et al. (2000) expressed by their integer k. The stellar tracks are distinguished by the mass M_o, which is equivalent to the ZAMS mass the star would have had without interaction. M_Hef and M_FGB are defined by Eqs. (2) and (3) from Hurley et al. (2000). M_Hef represents the maximum initial mass for which helium ignites degenerately in a helium flash, which is  ~2 M_⊙ for solar metallicities. M_FGB is the maximum initial mass for which helium ignites on the first giant branch, which is  ~13 M_⊙ for solar metallicities. M is the total mass of the star and M_c the mass of the core. HW87 represents Hjellming & Webbink (1987), who calculated ζ_ad for condensed polytropes, consisting of a compact core surrounded by an envelope with polytropic index n = 3/2. For stars on the first giant branch there are two prescriptions of ζ_ad. If the convective zone in the upper layers of the envelope is shallow (fits from Yungelson, priv. comm.), we assumed the envelope responds to mass loss in a similar manner as radiative envelopes.