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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 ![]() |
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Figure 2:
Some of our model photospheres (solid lines) are compared with those by
Plez et al. (1992) (dots).
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Figure 3:
a) Logarithmic abundance corrections for the lines of
the CO first overtone bands of ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 4:
a) Logarithmic abundance corrections for the lines of the
CO first and second overtone bands observed in ![]() ![]() ![]() ![]() ![]() |
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Figure 6:
a) Logarithmic abundance corrections for the lines of the
CO first and second overtone bands observed in ![]() ![]() ![]() ![]() ![]() |
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Figure 8:
a) Logarithmic abundance corrections for the lines of the
CO first and second overtone bands observed in ![]() ![]() ![]() ![]() ![]() |
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Figure 10:
a) Logarithmic abundance corrections for the lines of
OH fundamental bands observed in ![]() ![]() ![]() ![]() ![]() |
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Figure 12:
Lower excitation potentials (LEPs) of the lines
plotted against
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Figure 13:
a) Logarithmic abundance corrections for the lines of the OH
first overtone bands observed in ![]() ![]() ![]() ![]() ![]() |
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Figure 15:
The ordinate scale shows abundances of 12C16O
(first and second overtones by filled circles and
triangles, respectively), 13C16O (open squares), and
12C17O (open diamonds)
derived from the observed values of log ![]() ![]() ![]() |
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Figure 16:
Observed spectra are shown by dots. Some 12C16O
and 12C17O features are indicated by open and filled
triangles, respectively. Synthetic spectra with assumed
16O/17O ratios are shown by heavy solid lines while
those with null 17O value by light solid lines.
a) Observed spectrum of 10 Dra compared with the synthetic one with
16O/17O = 151.
b) Observed spectrum of RZ Ari compared with the
synthetic one with 16O/17O = 607.
c) Observed spectrum of ![]() |
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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 16O/17O ratios are plotted against stellar mass by filled circles and by the filled triangles if only lower limits can be estimated. Predicted 16O/17O ratios by FDU and SDU are shown by solid and dash-dotted lines, respectively. b) the observed 12C/13C ratios are plotted by filled circles against stellar mass. Dashed curve is the predicted 12C/13C 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
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Figure 7:
a) Confirmation of the null logarithmic abundance corrections
for log
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Figure 9:
a) Confirmation of the null logarithmic abundance corrections
for log
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Figure 11:
a) Confirmation of the null logarithmic abundance corrections
for log
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Figure 14:
a) Confirmation of the null logarithmic abundance corrections
for log
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