Formation of Carbon Dwarfs
Astrophysics
2012-01-30 v2
Abstract
We consider the formation of dwarf carbon stars via accretion from a carbon AGB companion in light of the new 107 object sample of Downes et al. (2004). This sample is now large enough to allow good mass determination via comparison of a composite spectrum to theoretical atmospheric models. Carbon dwarfs of spectral type M are indeed main sequence M dwarfs with enhanced metallicity and carbon abundance. We also calculate the predicted abundance of both M and of F/G carbon dwarfs, and show that the latter should be falsifiable in the near future.
Cite
@article{arxiv.astro-ph/0502152,
title = {Formation of Carbon Dwarfs},
author = {Charles L. Steinhardt and Dimitar D. Sasselov},
journal= {arXiv preprint arXiv:astro-ph/0502152},
year = {2012}
}
Comments
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