  We present spatially resolved high-resolution spectrophotometric data for the
planetary nebulae PB8, NGC2867, and PB6. We have analyzed two knots in NGC2867
and PB6 and one in PB8. The three nebulae are ionized by [WC] type nuclei:
early [WO] for PB6 and NGC2867 and [WC 5-6] in the case of PB8. Our aim is to
study the behavior of the abundance discrepancy problem (ADF) in this type of
PNe. We measured a large number of optical recombination (ORL) and
collisionally excited lines (CEL), from different ionization stages (many more
than in any previous work), thus, we were able to derive physical conditions
from many different diagnostic procedures. We determined ionic abundances from
the available collisionally excited lines and recombination lines. Based on
both sets of ionic abundances, we derived total chemical abundances in the
nebulae using suitable ionization correction factors. From CELs, we have found
abundances typical of Galactic disk planetary nebulae. Moderate ADF(O++) were
found for PB8 (2.57) and NGC2867 (1.63). For NGC2867, abundances from ORLs are
higher but still consistent with Galactic disk planetary nebulae. On the
contrary, PB8 presents a very high O/H ratio from ORLs. A high C/O was obtained
from ORLs for NGC2867; this ratio is similar to C/O obtained from CELs and with
the chemical composition of the wind of the central star, indicating that there
was no further C-enrichment in the star, relative to O, after the nebular
material ejection. On the contrary, we found C/O<1 in PB8. Interestingly, we
obtain (C/O)ORLs/(C/O)CELs < 1 in PB8 and NGC2867; this added to the similarity
between the heliocentric velocities measured in [OIII] and OII lines for our
three objects, argue against the presence of H-deficient metal-rich knots
coming from a late thermal pulse event.
