Poster abstract details

PNe around [WR] central stars constitute a particular photoionized nebula class, representing about 10\% of the PNe with known progenitor. They seem suitable for analyzing the abundance discrepancy found when abundances are derived from collisional excited lines in contrast with those from recombination lines, due to it is plausible to expect that some H-deficient material in small knots could be contaminating the hot plasma, which is one of the explanation proposed to explain large abundance discrepancy factors (ADFs). In this talk we present results obtained from the analysis of very deep echelle spectra of a dozen of planetary nebulae with central stars classified as weak emission lines stars (wels) or [WC] type stars.