Extremely Metal-poor Stars. The Carbon-rich, Neutron Capture Element--poor Object CS 22957-027

Details Extremely Metal-poor Stars. The Carbon-rich, Neutron Capture Element--poor Object CS 22957-027 Extremely Metal-poor Stars. The Carbon-rich, Neutron Capture Element--poor Object CS 22957-027

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...489l.169n&link_type=abstract

Astrophysical Journal Letters v.489, p.L169

Astronomy and Astrophysics

Astronomy

88

Nuclear Reactions, Nucleosynthesis, Abundances, Stars: Abundances, Stars: Carbon, Stars: Population Ii, Galaxy: Abundances

Scientific paper

Analysis of high-resolution spectra of the carbon-rich, metal-poor giant CS 22957-027 yields [Fe/H] = -3.38, [C/Fe] = 2.2, 12C/13C = 10, [N/Fe] = 2.0, [Sr/Fe] = -0.6, and [Ba/Fe] = -1.0. This combination of large C and N overabundances and the absence of heavy neutron capture element enrichment differs from that normally found in C-rich metal-poor stars, which are all usually enhanced in these elements. Any explanation in terms of the canonical binary mass transfer origin of CH stars or of supernovae ejecta requires a decoupling of the processes that produce the C and neutron capture element overabundances. An alternative possibility is that the heavy element abundances are typical of the halo interstellar medium from which CS 22957-027 formed and the C and N overabundances result from processes internal to the star itself. One candidate process is helium core flash induced mixing in low-mass, zero heavy element stars as predicted by Hollowell et al. CS 22957-027 exhibits strong features of 13CH at ~4019.0 A, which coincide with Th II 4019.12 A. This should be borne in mind when using the Th/Eu ratio in metal-poor, C-rich stars such as CS 22892-052 as a Galactic chronometer.

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