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Confrontation of the ISO spectra with model atmospheres
of M-type stars:
dwarfs, giants, and supergiants
T. Tsuji, W. Aoki, - K. Ohnaka
Institute of Astronomy, The University of Tokyo
The ISO spectra provide unique opportunity not only to test
the model atmospheres of cool stars but also to explore new problems on
the atmospheric structure of cool stars.
First, we hope to clarify what can be understood by the present model
atmospheres, which can now be regarded as well developed within
the framework of the classical theory. Especially, recent
release of the extensive spectral line database such as HITEMP is quite
timely in exploring the full details of the ISO spectra by means
of the model atmospheres. We also hope to clarify the luminosity effects
in the infrared spectra of cool stars by our observations of dwarfs,
giants, and supergiants with the ISO, and to calibrate these spectra
in terms of the basic stellar parameters by the use of our grids of
models that cover a wide range of temperature and luminosity.
However, we already found that the classical photospheric models
are not sufficient to understand full details of the ISO spectra, even
in the near IR, and more unified understanding of the outer atmosphere
should be needed for this purpose.
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