Figure 1: Program stars shown by filled circles on the HR diagram and recent evolutionary tracks (Claret 2004) shown by grey lines. Stellar masses (in unit of solar mass ) are indicated on some evolutionary tracks. | |
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Figure 2: Some of our model photospheres (solid lines) are compared with those by Plez et al. (1992) (dots). , , log g, and are as follows. A: 1.0/2750/-0.50/295, B: 1.0/3200/0.00/166, and C: 2.0/3600/0.50/132. | |
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Figure 3: a) Logarithmic abundance corrections for the lines of the CO first overtone bands of Her plotted against the observed log values for assumed values of , 3.5, and 4.0 km s^{-1}. The analysis outlined in Sect. 3 is applied to the lines of log (filled circles) with our model b/2.0/150/3200. b) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, which are the solution of the line-by-line analysis of Her in a). | |
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Figure 4: a) Logarithmic abundance corrections for the lines of the CO first and second overtone bands observed in Her plotted against the observed values for assumed values of , 3.0, and 3.6 km s^{-1}. The CO lines of the first and second overtone bands are shown by circles and triangles, respectively (model photosphere: b/2.0/150/3300). b) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, which are the solution of the line-by-line analysis of the weak lines (filled symbols) in a). | |
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Figure 6: a) Logarithmic abundance corrections for the lines of the CO first and second overtone bands observed in Peg plotted against the observed values for assumed values of , 2.0, and 2.4 km s^{-1} (model: a/2.0/100/3600). b) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, which are the solution of the line-by-line analysis of the weak lines (filled symbols) in a). | |
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Figure 8: a) Logarithmic abundance corrections for the lines of the CO first and second overtone bands observed in Per plotted against the observed values for assumed values of , 3.5, and 4.0 km s^{-1} (model: b/2.0/100/3500). b) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, which are the solution of the line-by-line analysis of the weak lines (filled symbols) in a). | |
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Figure 10: a) Logarithmic abundance corrections for the lines of OH fundamental bands observed in Her plotted against the observed values for assumed values of , 3.0, and 4.0 km s^{-1} (model: b/2.0/150/3300). b) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, which are the solution of the line-by-line analysis of the weak lines (filled circles) in a). | |
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Figure 12: Lower excitation potentials (LEPs) of the lines plotted against values. a) CO first overtone bands observed in Her. b) OH fundamental bands observed in Her. | |
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Figure 13: a) Logarithmic abundance corrections for the lines of the OH first overtone bands observed in Per plotted against the observed values for assumed values of , 3.0, and 4.0 km s^{-1} (model: b/2.0/100/3500). b) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, which are the solution of the line-by-line analysis of the weak lines (filled circles) in a). | |
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Figure 15: The ordinate scale shows abundances of ^{12}C^{16}O (first and second overtones by filled circles and triangles, respectively), ^{13}C^{16}O (open squares), and ^{12}C^{17}O (open diamonds) derived from the observed values of log in the abscissa. a) 10 Dra. Note that there are three lines of ^{13}C^{16}O and ^{12}C^{17}O, of which two are overlapping in the plot. b) RZ Ari. c) Oph. d) Gem. | |
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Figure 16: Observed spectra are shown by dots. Some ^{12}C^{16}O and ^{12}C^{17}O features are indicated by open and filled triangles, respectively. Synthetic spectra with assumed ^{16}O/^{17}O ratios are shown by heavy solid lines while those with null ^{17}O value by light solid lines. a) Observed spectrum of 10 Dra compared with the synthetic one with ^{16}O/^{17}O = 151. b) Observed spectrum of RZ Ari compared with the synthetic one with ^{16}O/^{17}O = 607. c) Observed spectrum of Aqr compared with the synthetic one with ^{16}O/^{17}O = 1000. d) Observed spectrum of RR UMi compared with the synthetic one with ^{16}O/^{17}O = 2000. | |
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Figure 17: Observed abundances of a) carbon (Table 6), b) nitrogen (Aoki & Tsuji 1997; Table 6), c) oxygen (Table 6; if the results derived from the H and L band spectra are available, mean values are used), and d) C + N + O, compared with the predictions of evolutionary models (Claret 2004). The results of FDU and SDU for the case of Z = 0.02 are shown by solid and dash-dotted lines, respectively, in each panel. The observed C + N + O abundances are smaller by about 0.16 dex compared with the predictions based on Z = 0.02 as can be seen in panel d). This initial metallicity correction of -0.16 dex is applied to the predicted C, N, and O abundances in panels a), b), and c), respectively, and the corrected results are shown by dashed lines. In each panel, the solar abundances are shown by open square (Anders & Grevesse 1989; Ayres et al. 2006) and by open diamond (Allende Prieto et al. 2002). | |
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Figure 18: a) The observed ^{16}O/^{17}O ratios are plotted against stellar mass by filled circles and by the filled triangles if only lower limits can be estimated. Predicted ^{16}O/^{17}O ratios by FDU and SDU are shown by solid and dash-dotted lines, respectively. b) the observed ^{12}C/^{13}C ratios are plotted by filled circles against stellar mass. Dashed curve is the predicted ^{12}C/^{13}C ratios by the ``Compulsory Deep Mixing (CDM: Eggleton et al. 2008)''. | |
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Figure 5: a) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, resulting from the line-by-line analysis of the weak lines of CO in Lyr (model: b/2.0/150/3400). b) The same as a) but for log and km s^{-1} in 30g Her (model: b/2.0/150/3300). c) The same as a) but for log and km s^{-1} in RX Boo (model: b/2.0/250/2900). | |
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Figure 7: a) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, resulting from the line-by-line analysis of the weak lines of CO in Tau (model: a/2.0/50/3900). b) The same as a) but for log and km s^{-1} in Vir (model: a/2.0/75/3800). c) the same as a) but for log and km s^{-1} in Cet (model: a/2.0/50/3900). | |
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Figure 9: a) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, resulting from the line-by-line analysis of the weak lines of CO in Eri (model: a/2.0/75/3700). b) The same as a) but for log and km s^{-1} in R Lyr (model: b/2.0/150/3300). c) The same as a) but for log and km s^{-1} in SW Vir (model: b/2.0/250/2900). | |
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Figure 11: a) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, resulting from the line-by-line analysis of the weak lines of OH in Tau (model: a/2.0/50/3900). b) The same as a) but for log and km s^{-1} in R Lyr (model: b/2.0/150/3300). c) The same as a) but for log and km s^{-1} in SW Vir (model: b/2.0/250/2900). | |
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Figure 14: a) Confirmation of the null logarithmic abundance corrections for log and km s^{-1}, resulting from the line-by-line analysis of the weak lines of OH in Tau (model: a/2.0/50/3900). b) The same as a) but for log and km s^{-1} in Lib (model: a/2.0/100/3600). c) the same as a) but for log and km^{-1} in R Lyr (model: b/2.0/150/3300). | |
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