![]() 2006, Stars and Nuclei: A Tribute to Manuel Forestini, Eds T. We tend to propose a reaction network of a nuclear cycle namely carbon–nitrogen–oxygen–fluorine (CNOF) at evolved stellar condition since fluorine \((^\), edited by C. ![]() The proton-capture reactions are presently recognised in concert of the necessary candidates for that sort of observed behaviour in the second generation stars. We found that the relative abundance of is generally large in red symbiotic systems.The origin of the abundance pattern and also the (anti)correlation present among the elements found in stars of globular clusters (GCs) remains unimproved until date. This was confirmed in a number of objects by the low 12C/ 13C ratio (5-23). The enrichment in 14N isotope, found in all these objects, indicates that the giants have experienced the first dredge-up. Our analysis reveals metallicities distributed in a wide range from slightly supersolar ( ∼ +0.35 dex) to significantly subsolar ( ∼ -0.8 dex) but principally with near-solar and slightly subsolar metallicity ( ∼ -0.4 to -0.3 dex). Spectrum synthesis methods employing standard local thermal equilibrium analysis and atmosphere models were used to obtain photospheric abundances of CNO and elements around the iron peak (Fe, Ti, Ni, and Sc). Here we present results for 24 S-type systems. This is the third in a series of papers on the chemical composition of symbiotic giants determined from high-resolution (R ∼ 50 000), near-infrared spectra. However, the number of symbiotic giants with fairly well determined photospheric composition is still insufficient for statistical analyses. The elemental abundances of symbiotic giants are essential to address the role of chemical composition in the evolution of symbiotic binaries, to map their parent population, and to trace their mass transfer history.
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