Double white dwarf mergers and elemental surface abundances in extreme helium and R Coronae Borealis stars

TL;DR

This paper models the surface abundances of extreme helium and R Coronae Borealis stars as resulting from white dwarf mergers, examining nucleosynthesis processes and progenitor star characteristics to explain observed elemental compositions.

Contribution

It introduces a detailed merger model considering layered white dwarf structures and explores nucleosynthesis during mergers to explain surface abundances in EHe and RCB stars.

Findings

High carbon and oxygen abundances may result from dredge-up or alpha-burning during mergers.

Large O18 quantities could originate from post-AGB models or merger processes.

Progenitor stars likely had initial masses between 1.9 and 3 solar masses.

Abstract

The surface abundances of extreme helium (EHe) and R Coronae Borealis (RCB) stars are discussed in terms of the merger of a carbon-oxygen white dwarf with a helium white dwarf. The model is expressed as a linear mixture of the individual layers of both constituent white dwarfs, taking account of the specific evolution of each star. In developing this recipe from previous versions, particular attention has been given to the inter-shell abundances of the asymptotic giant branch star which evolved to become the carbon-oxygen white dwarf. Thus the surface composition of the merged star is estimated as a function of the initial mass and metallicity of its progenitor. The question of whether additional nucleosynthesis occurs during the white dwarf merger has been examined. The high observed abundances of carbon and oxygen must either originate by dredge-up from the core of the carbon-oxygen white dwarf during a cold merger or be generated directly by alpha-burning during a hot merger. The presence of large quantities of O18 may be consistent with both scenarios, since a significant O18 pocket develops at the carbon/helium boundary in a number of our post-AGB models. The production of fluorine, neon and phosphorus in the AGB intershell produces n overabundance at the surface of the merged stars, but generally not in sufficient quantity. However, the evidence for an AGB origin for these elements points to progenitor stars with initial masses in the range 1.9 - 3 solar masses. There is not yet sufficient information to discriminate the origin (fossil or prompt) of all the abundance anomalies observed in EHe and RCB stars. Further work is required on argon and s-process elements in the AGB intershell, and on the predicted yields of all elements from a hot merger.