White dwarf mergers and the origin of R Coronae Borealis stars
P. Lor\'en-Aguilar, R. Longland, J. Jos\'e, E. Garc\'ia-Berro, L.G., Althaus, J. Isern
TL;DR
This study models the merger of helium and carbon-oxygen white dwarfs to explain the chemical abundances observed in R Coronae Borealis stars, focusing on nucleosynthesis outcomes.
Contribution
It provides a detailed nucleosynthesis analysis of white dwarf mergers, linking merger dynamics to observed stellar compositions.
Findings
Chemical abundance patterns match observed R Coronae Borealis stars.
Oxygen and fluorine abundances are qualitatively consistent with observations.
The merger scenario explains the origin of R Coronae Borealis stars.
Abstract
We present a nucleosynthesis study of the merger of a 0.4 solar masses helium white dwarf with a 0.8 solar masses carbon-oxygen white dwarf, 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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Taxonomy
TopicsGamma-ray bursts and supernovae · Stellar, planetary, and galactic studies · Astronomy and Astrophysical Research