However, this is not required for the binaries considered in this work. Due to the exponential dependence of the mass transfer rate on the stellar radius, an explicit scheme for computing the mass transfer rate can easily lead to numerical instabilities. However, for each iteration a complete stellar model needs to be computed. The change of the orbital period due to the mass transfer and stellar wind mass loss is computed according to Podsiadlowski et al. The spin angular momentum of both stars is neglected.
Mass transfer is treated quasi conservatively.
The only mass loss from the system is due to the stellar winds of both components. This mixing process is important in stars which accrete helium-enriched material. Table 3 in Sect. In this system, the secondary star ends its evolution first. The time of its supernova explosion marks the end of the solid line in the track of the primary.