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Effective Temperature Scales of Red Giant Stars

Published online by Cambridge University Press:  25 May 2016

David R. Alexander
Affiliation:
Dept. of Physics, Wichita State University, Wichita, KS 67260–0032, USA
Jason W. Ferguson
Affiliation:
Dept. of Physics, Wichita State University, Wichita, KS 67260–0032, USA
Robert F. Wing
Affiliation:
Astronomy Dept., Ohio State University, Columbus, OH 43210, USA
Hollis R. Johnson
Affiliation:
Dept. of Astronomy, Indiana University, Bloomington, IN 47405, USA
Peter H. Hauschildt
Affiliation:
Dept. of Physics, Wichita State University, Wichita, KS 67260–0032, USA
France Allard*
Affiliation:
Dept. of Physics, Wichita State University, Wichita, KS 67260–0032, USA
*
1 Now at CRAL, Ecole Normale Superieure, Lyon, 69364 France Cedex 07

Abstract

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We have completed a grid of spherically symmetric AGB star atmospheres using the state of the art spectral synthesis code PHOENIX. Models are constructed for stars with masses of 1 M and 1.5 M, spanning the range 10 to 3300 L in luminosity and 2500 to 5200 K in effective temperature. We find that grains of Al2O3 and CaTiO3 among other species form in atmospheres cooler than Teff = 3000 K. In the coolest models the grains cause a weakening of the TiO absorption features in the red and near infrared of up to 30% through both a depression of the continuum and a depletion of the TiO number abundance. We use spectrophotometric observations from a number of catalogs to determine effective temperature – spectral class and effective temperature – color relationships. We also compare synthetic colors calculated from our models with observations of M giants on Wing's 8-color narrow-band system of classification photometry.

Type
Part 1. Basic Facts, Structure, Evolution, Nucleosynthesis
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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