Abundance similarities between the R CrB star V854 Cen and the born-again Sakurai's object

TL;DR

This study compares the elemental abundances of the R CrB star V854 Cen with Sakurai's object, suggesting a shared evolutionary origin linked to the final helium-shell flash, which supports a possible formation scenario for R CrB stars.

Contribution

It provides the first detailed chemical comparison between V854 Cen and Sakurai's object, proposing a common evolutionary pathway involving the final helium-shell flash.

Findings

V854 Cen closely resembles Sakurai's object in chemical composition.

V854 Cen shows no clear signs of dust-gas separation typical in post-AGB stars.

The abundance similarities support a final-flash origin for V854 Cen and possibly other R CrB stars.

Abstract

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.