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A nova re-accretion model for J-type carbon stars

Sengupta, S., Izzard, Robert and Lau, H. H. B. (2013) A nova re-accretion model for J-type carbon stars Astronomy & Astrophysics, 559.

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The J-type carbon (J)-stars constitute 10–15% of the observed carbon stars in both our Galaxy and the Large Magellanic Cloud (LMC). They are characterized by strong absorption bands with low 12C/13C ratios along with other chemical signatures peculiar for typical carbon stars, e.g. a lack of s-process enhancement. Most of the J-stars are dimmer than the N-type carbon stars some of which, by hot-bottom burning, make only in a narrow range of masses. We investigate a binary-star formation channel for J-stars involving re-accretion of carbon-rich nova ejecta on main-sequence companions to low-mass carbon-oxygen white-dwarfs. The subsequent evolution of the companion stars in such systems is studied with a rapid binary evolutionary code to predict chemical signatures of nova pollution in systems which merge into giant single stars. A detailed population synthesis study is performed to estimate the number of these mergers and compare their properties with observed J-stars. Our results predict that such nova polluted mergers evolve with low luminosities as well as low 12C/13C ratios like the majority of observed J-stars (e.g. in the LMC) but cannot account for the observed fraction of J-stars in existing surveys of carbon stars.

Item Type: Article
Divisions : Faculty of Engineering and Physical Sciences > Physics
Authors :
Sengupta, S.
Lau, H. H. B.
Date : 15 November 2013
DOI : 10.1051/0004-6361/201322420
Depositing User : Karen Garland
Date Deposited : 04 Oct 2018 15:37
Last Modified : 04 Oct 2018 15:37

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