Figure 1

Figure 1: Descendants of components of close binaries depending on the radius of the star at RLOF. The boundary between progenitors of He and CO-WDs is uncertain by several 0.1 M ⊙, the boundary between WDs and NSs by ∼ 1M ⊙, while for the formation of BHs the lower mass limit may be even by ∼ 10M ⊙ higher than indicated.