Nucleosynthesis during the Merger of White Dwarfs and the Origin of R Coronae Borealis Stars

Details Nucleosynthesis during the Merger of White Dwarfs and the Origin of R Coronae Borealis Stars Nucleosynthesis during the Merger of White Dwarfs and the Origin of R Coronae Borealis Stars

2011-07-12

arxiv.org/abs/1107.2233v2

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

5 Pages, 2 figures. Accepted to Astrophysical Journal Letters; http://stacks.iop.org/2041-8205/737/L34

Scientific paper

10.1088/2041-8205/737/2/L34

Many hydrogen deficient stars are characterised by surface abundance patterns that are hard to reconcile with conventional stellar evolution. Instead, it has been suggested that they may represent the result of a merger episode between a helium and a carbon-oxygen white dwarf. In this Letter, we present a nucleosynthesis study of the merger of a 0.4 M_sol helium white dwarf with a 0.8 M_sol carbon-oxygen white dwarf, by coupling the thermodynamic history of Smoothed Particle Hydrodynamics particles with a post-processing code. The resulting chemical abundance pattern, particularly for oxygen and fluorine, is in qualitative agreement with the observed abundances in R Coronae Borealis stars.

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