Query : 2013A&A...559A..66S

2013A&A...559A..66S - Astronomy and Astrophysics, volume 559A, 66-66 (2013/11-1)

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


Abstract (from CDS):

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 13C 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 13C 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.

Abstract Copyright:

Journal keyword(s): stars: carbon - stars: chemically peculiar - novae, cataclysmic variables - white dwarfs - stars: abundances - stars: statistics

Simbad objects: 4

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Number of rows : 4
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
1 V* WZ Cas C* 00 01 15.8567946264 +60 21 19.025920224 8.77 9.47 7.13     C-N7III: 315 0
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 17261 1
3 V* BM Gem C* 07 20 59.0073521904 +24 59 58.086063708     11.50     C-J5- 149 1
4 V* V842 Cen No* 14 35 52.5683885352 -57 37 35.391092232           ~ 146 0

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