Table 2: Surface abundances of the models presented in Sect. 4. Abundances are taken at the moment the models reach the giant region for the first time after the VLTP. Abundances from Lawlor & Macdonald (2003) are taken from models of similar metallicity (z=0.02).
  H He C N O $M^{{\rm total}}_{\rm H}/M_\odot$
MLT (early VLTP) $3.7 \times 10^{-4}$ 0.324 0.371 0.0145 0.217 $3.19 \times 10^{-6}$
MLT (f=0.03) $5\times 10^{-6} $ 0.307 0.378 0.0129 0.229 $7.24 \times 10^{-9}$
GNA ( $\nabla\mu=0$) $3.2\times 10^{-5} $ 0.316 0.378 0.0129 0.221 $2.19 \times 10^{-7}$
GNA $3.3\times 10^{-5} $ 0.316 0.378 0.0127 0.221 $6.76 \times10^{-9}$
Lawlor $D/10^{-4}\dagger$ 0.06 0.57 0.26 - 0.07 $2 \times10^{-6}$
Lawlor $D/10^{-3}\dagger$ 0.02 0.55 0.28 - 0.08 $3 \times10^{-7}$
Lawlor $D/10^{-2}\ddagger$ 0.04 0.54 0.28 - 0.08 -
Herwig (1999) - 0.388 0.362 - 0.219 $4 \times 10^{-11}$
Most PG1159 pulsators - 0.397 0.357 0.0139 0.159 -
PG1159-035 - 0.287 0.516 0.0100 0.115 -
$\dagger$ Abundances correspond to the moment at which the star reaches the WD cooling track. $\ddagger$ Abundances correspond to the first return to the giant region, where the envelope was homogeinized by mixing. In the last column the values of the total amount of H in the star after the VLTP are presented. Relative abundances of PG1159 stars are taken from Dreizler & Heber (1998) and normalized to the total amount of  $\rm C+O+N+He$ given by the models.

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