Locations of O(He) stars (red, Reindl et al. 2014; Werner et al. 2014; Wassermann et al. 2010; De Marco et al. 2014), PG 1159 stars (black, Geier et al. in prep.; Werner et al. 2014; Gianninas et al. 2010; Werner & Herwig 2006; Schuh et al. 2008) and DO WDs (purple, this work, Werner et al. 2014; Mahsereci 2011; Hügelmeyer et al. 2006; Dreizler & Werner 1996; Nagel et al. 2006) in the log T_eff–log g plane compared to VLTP post-AGB (solid lines) evolutionary tracks (labeled with stellar masses in M_⊙) of Althaus et al. (2009). The black solid and dashed lines indicate theoretical wind limits for abundance changes as predicted by Unglaub & Bues (2000) and discussed in Sect. 4.2.