Carbon-Enhanced Metal-Poor (CEMP) stars

Details Carbon-Enhanced Metal-Poor (CEMP) stars Carbon-Enhanced Metal-Poor (CEMP) stars

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010iaus..265..111a&link_type=abstract

Chemical Abundances in the Universe: Connecting First Stars to Planets, Proceedings of the International Astronomical Union, IAU

Astronomy and Astrophysics

Astronomy

4

Stars:Abundances, Stars:Agb And Post-Agb, Stars:Carbon, Supernovae

Scientific paper

A significant fraction of metal-poor stars have large over-abundances of carbon, and are called Carbon-Enhanced Metal-Poor (CEMP) stars. Most of CEMP stars also show excesses of heavy neutron-capture elements like Ba, indicating that their origin is the nucleosynthesis in AGB stars. Remaining CEMP stars that have Ba abundances as low as non-carbon-rich stars appear in the lowest metallicity range ([Fe/H]≲-2.5), and connections with the two most iron-deficient stars (so-called Hyper Metal-Poor stars) are suggested. Although the origins of the carbon-excesses in these objects have not been well identified, some objects suggest contributions of faint supernovae. Remaining problems on CEMP stars, such as the binary fraction, excess of r-process elements, are discussed.

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