Stellar mass loss cannot be predicted by stellar tracks. In particular, we plan to use them to analyze the thousands of spectra which will be provided by the forthcoming Medium Resolution Spectroscopic Survey with LAMOST Zhao et al. Related articles in Web of Science Google Scholar. Citing articles via Web of Science Morossi 1 , P. This behaviour ought to be expected and is a direct consequence of the empirical stellar library, in which stellar parameter space is inevitably sampled worse at the ends of the distribution. For comparison purposes let us divide the description of the indices into two temperature intervals.
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This index has been defined in Thomas et al. Same diagram as in Figure 4 for the GCs of the merger remnant galaxy NGC filled symbols. The figure shows an overall consistency of observed colors with those predicted for main-sequence stars of spectral types G and K. Castelli , private communication , computed with updated Opacity Distribution Functions hereafter newODFs , were adopted in the following ranges of atmospheric parameters. The star HD has a peculiar spectrum since there are regions that are in significant disagreement with the prediction of the synthetic models see Figure 16 c. A fundamental step from the observational point of view in the knowledge of the Milky Way stellar content has been accomplished with the SDSS York et al.