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Fig. 8.
HR diagram of H-poor CSPNe, according subtype. H-deficient tracks correspond to the post-VLTP sequences computed by Miller Bertolami & Althaus (2006), which display He, C, and O photospheric abundances similar to those of [WR]-CSPNe and PG 1159 stars (MCSPN = 0.515, 0.542, 0.584, 0.664 and 0.870 M⊙, from right to left).
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