Notes. The mass of the systems is assumed to be , where represents the initial donor’s mass closest to the actual m_star in Ge et al. (2020) tables. Comparison to our results is made using the circularised orbital period as in Eq. (31), for eccentric systems with e >  0. The estimate of is reported with the same significant digits as the eccentricities in Table 1. The hypothesized channels of purely isotropic re-emission, β = 1, and mass outflow from L₂ with efficiency υ = 0.75 are both considered. The outcomes are also labeled to argue whether the systems have a set of initial properties that can lead to the evolution into merging double COs via stable MT (GW merger), or are expected to evolve into a wide binary (wide binary) or undergo unstable MT (unstable MT).