  The elemental abundances of the mildly hydrogen-deficient R Coronae Borealis
(R CrB) star V854 Cen have been estimated. The R CrB stars have been divided
into majority and minority classes judging by their abundance patterns. Class
assignment has previously been unambiguous but V854 Cen has traits of both the
minority and majority class. Neither V854 Cen nor the three obvious minority
members show any clear abundance signatures of having been affected by e.g.
dust-gas separation as often observed in post-AGB stars. By chemical
composition, V854 Cen closely resembles Sakurai's object, which has probably
recently experienced a final He-shell flash. Therefore V854 Cen and Sakurai's
object may share the same evolutionary background, which would add support for
the final-flash scenario as a viable origin of the R CrB stars. Most of the few
differences in abundance ratios between the stars could if so be attributed to
milder H-ingestion in connection with the final He-shell flash of V854 Cen. The
identification of either the majority or the minority group, if any, as final
flash objects, remain uncertain, however, due to the unclear membership status
of V854 Cen.
