Abstract
Observational results pertaining to the thermal and dynamical structure of the atmospheres of cool, evolved stars are summarized. It is noted that the inferred atmospheric properties of a given star of this type appear to depend on its position relative to the various dividing lines which have been identified in the HR diagram. Using computed evolutionary models, changes in the internal structure of an intermediate mass star are followed as its redward motion in the HR diagram carries it across the transition region dividing line. It is suggested that this boundary may reflect the onset of deep envelope convection during post main sequence evolution.
The National Center for Atmospheric Research is sponsored by the National Science Foundation.
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MacGregor, K.B. (1987). Stars with thin and thick convection zones:M giants. In: Linsky, J.L., Stencel, R.E. (eds) Cool Stars, Stellar Systems, and the Sun. Lecture Notes in Physics, vol 291. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-18653-0_139
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DOI: https://doi.org/10.1007/3-540-18653-0_139
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