Reproducing the observed abundances in RCB and HdC stars with post-double degenerate merger models – constraints on merger and post-merger simulations and physics processes

Дата и время публикации : 2012-11-14T19:47:08Z

Авторы публикации и институты :
Athira Menon
Falk Herwig
Pavel A. Denissenkov
Geoffrey C. Clayton
Jan Staff
Marco Pignatari
Bill Paxton

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: accepted for publication in ApJ
Первичная категория: astro-ph.SR

Все категории : astro-ph.SR

Краткий обзор статьи: The R Coronae Borealis (RCB) stars are hydrogen-deficient, variable stars that are most likely the result of He-CO WD mergers. They display extremely low oxygen isotopic ratios, 16O/18O ~ 1 – 10, 12C/13C>=100, and enhancements up to 2.6dex in F and in s-process elements from Zn to La, compared to solar. These abundances provide stringent constraints on the physical processes during and after the double-degenerate merger. As shown before O-isotopic ratios observed in RCB stars cannot result from the dynamic double-degenerate merger phase, and we investigate now the role of the long-term 1D spherical post-merger evolution and nucleosynthesis based on realistic hydrodynamic merger progenitor models. We adopt a model for extra envelope mixing to represent processes driven by rotation originating in the dynamical merger. Comprehensive nucleosynthesis post-processing simulations for these stellar evolution models reproduce, for the first time, the full range of the observed abundances for almost all the elements measured in RCB stars: 16O/18O ratios between 9 and 15, C-isotopic ratios above 100, and ~1.4 – 2.35dex F enhancements, along with enrichments in s-process elements. The nucleosynthesis processes in our models constrain the length and temperature in the dynamic merger shell-of-fire feature as well as the envelope mixing in the post-merger phase. s-process elements originate either in the shell-of-fire merger feature or during the post-merger evolution, but the contribution from the AGB progenitors is negligible. The post-merger envelope mixing must eventually cease ~ 10^6yr after the dynamic merger phase, before the star enters the RCB phase.

Category: Physics