Stellar post asymptotic giant branch ( post-AGB ) evolution can be completely altered by a final thermal pulse ( FTP ) which may occur when the star is still leaving the AGB ( AFTP ) , at the departure from the AGB at still constant luminosity ( late TP , LTP ) or after the entry to the white-dwarf cooling sequence ( very late TP , VLTP ) . Then convection mixes the He-rich material with the H-rich envelope . According to stellar evolution models the result is a star with a surface composition of \mathrm { H } \approx 20 % by mass ( AFTP ) , \approx 1 % ( LTP ) , or ( almost ) no H ( VLTP ) . Since FTP stars exhibit intershell material at their surface , spectral analyses establish constraints for AGB nucleosynthesis and stellar evolution . We performed a spectral analysis of the so-called hybrid PG 1159-type central stars ( CS ) of the planetary nebulae Abell 43 and NGC 7094 by means of non-local thermodynamical equilibrium models . We confirm the previously determined effective temperatures of \mbox { $T _ { \mathrm { eff } } $ } \hskip { -1.422638 pt } = \hskip { -1.422638 pt } 115 000 \pm 5 % 000 \mathrm { K } and determine surface gravities of \log ( g / \mathrm { cm / s ^ { 2 } } ) = 5.6 \pm 0.1 for both . From a comparison with AFTP evolutionary tracks , we derive stellar masses of 0.57 ^ { +0.07 } _ { -0.04 } M _ { \odot } and determine the abundances of H , He , and metals up to Xe . Both CS are likely AFTP stars with a surface H mass fraction of 0.25 \pm 0.03 and 0.15 \pm 0.03 , respectively , and a Fe deficiency indicating subsolar initial metallicities . The light metals show typical PG 1159-type abundances and the elemental composition is in good agreement with predictions from AFTP evolutionary models . However , the expansion ages do not agree with evolution timescales expected from the AFTP scenario and alternatives should be explored .