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The modelling of M-giant spectra

Published online by Cambridge University Press:  25 May 2016

Bertrand Plez
Bertrand Plez*
Affiliation:
Astronomiska observatoriet, box 515, S-75120 Uppsala and Atomspektroskopi, Fysiska inst., box 118, S-221 00 Lund, Sweden
*
1present address: GRAAL, Université Montpellier 11, 34095 Montpellier cedex 5, France

Abstract

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I review the current status of cool O-rich giant star spectral modelling, stressing some specific problems like line profiles and molecular data completeness. I discuss recent progress in molecular line lists (TiO, VO) and describe recent attempts in modelling normal M-giants as well as AGB star spectra, using static and hydrodynamic models. I anticipate further advances in the near future, with better radiative transfer in hydrodynamic models, that will allow detailed comparisons of models and observations, opening the possibility of deriving stellar parameters from spectroscopic and interferometric observations.

Type
Part 1. Basic Facts, Structure, Evolution, Nucleosynthesis
Information
Symposium - International Astronomical Union , Volume 191: Asymptotic Giant Branch Stars , 1999 , pp. 75 - 83
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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