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We present a detailed abundance analysis of 23 elements for a newlydiscovered carbon-enhanced metal-poor (CEMP) star, HE 0414-0343, from theChemical Abundances of Stars in the Halo (CASH) Project. Its spectroscopicstellar parameters are Teff = 4863 K, log g = 1.25, vmic = 2.20 km/s, and[Fe/H] = -2.24. Radial velocity measurements covering seven years indicate HE0414-0343 to be a binary. HE 0414-0343 has [C/Fe] = 1.44 and is stronglyenhanced in neutron-capture elements but its abundances cannot be reproduced bya solar-type s-process pattern alone. Traditionally, it could be classified as"CEMP-r/s" star. Based on abundance comparisons with AGB star nucleosynthesismodels, we suggest a new physically-motivated origin and classification schemefor CEMP-s stars and the still poorly-understood CEMP-r/s. The new schemedescribes a continuous transition between these two so-far distinctly treatedsubgroups: CEMP-sA, CEMP-sB, and CEMP-sC. Possible causes for a continuoustransition include the number of thermal pulses the AGB companion underwent,the effect of different AGB star masses on their nucleosynthetic yields, andphysics that is not well approximated in 1-D stellar models such as protoningestion episodes and rotation. Based on a set of detailed AGB models, wesuggest the abundance signature of HE 0414-0343 to have arisen from a >1.3 Msunmass AGB star and a late-time mass transfer, that transformed HE 0414-0343 intoa CEMP-sC star. We also find the [Y/Ba] ratio well parametrizes theclassification and can thus be used to easily classify any future such stars.

astrophysical journal/the astrophysical journal

The Chemical Abundances of Stars in the Halo (CASH) Project. III. A New  Classification Scheme for Carbon-Enhanced Metal-poor Stars with S-process  Element Enhancement