Elemental abundances of carbon, nitrogen, and oxygen in carbon stars

The elemental abundances of carbon, nitrogen, and oxygen in three carbon st ars (TX Psc, V Aql, and BL Ori) are determined from high-resolution infrare d spectra in a self-consistent manner, with the dependence of the atmospher ic structure on the chemical composition fully taken into account. For this purpose, we have constructed a grid of line-blanketed model atmospheres us ing a revised Band Model opacity. The derived carbon, nitrogen, and oxygen abundances show good agreement wit h the result obtained by Lambert et al. (1986) in most cases. The differenc es between the two groups are typically within 0.1 dex, which is remarkable for abundance analyses, especially for very cool stars. Since our model at mospheres and the method of the analysis are independent of their work, thi s result lends a support to the consistency of the analyses by the both gro ups. However, accurate determination of C/O ratio has turned out to be extremely difficult. The C/O ratios which are derived even with the same stellar par ameters with those adopted by Lambert et al. (1986) are somewhat larger tha n their results. 1.07 (TX Psc), 1.47 (V Aql), and 1.07 (BL Ori), while thei r results are 1.027 (TX Psc), 1.25 (V Aql), and 1.039 (BL Ori). Moreover. t he resulting abundances are rather sensitive to the effective temperature a nd the surface gravity. It is possible that the effective temperature scale is higher by 100 - 200 K than that Lambert et al. (1986) adopted, and in t hat case, C/O ratios in three stars become still systematically higher than those derived by Lambert et al. (1986), showing a contrast to their conclu sion that the majority of carbon stars have C/O ratios rather close to 1. I n fact, the C/O ratios derived here are 1.17 (TX Psc), 1.74 (V Aql), and 1. 19 (BL Ori). A decrease of the surface gravity from log g = 0.0 to - 0.5 al so leads to an increase of C/O ratio by 10%. In other words, given the unce rtainties of stellar parameters and molecular data in addition to internal errors, it is still difficult to determine C/O ratios within accuracy of 10 %, which can be translated to a difference between C/O = 1.02 and 1.1. The C-12/C-13 ratios in N-type carbon stars derived in our previous analysi s have been revised with the new model grid. The C-12/C-13 ratios in three stars have turned out to be 31 (TX Psc), 74 (V Aql), and 35 (BL Ori), large r by about 40% than those we obtained previously. And the C/O ratios and th e C-12/C-13 ratios derived here fall within the range predicted by the addi tion of C-12 to the atmosphere of K and M giants. It supports the scenario in which K and M giants evolve to carbon stars as C-12 synthesized in the t hermal pulse is dredged-up.