Hostname: page-component-6bf8c574d5-gr6zb Total loading time: 0 Render date: 2025-02-21T03:38:55.649Z Has data issue: false hasContentIssue false
  • English
  • Français

Effective Temperature Scales of Red Giant Stars

Published online by Cambridge University Press:  25 May 2016

David R. Alexander ,
Jason W. Ferguson ,
Robert F. Wing ,
Hollis R. Johnson ,
Peter H. Hauschildt  and
France Allard
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
*
1Now at CRAL, Ecole Normale Superieure, Lyon, 69364 France Cedex 07

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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
Information
Symposium - International Astronomical Union , Volume 191: Asymptotic Giant Branch Stars , 1999 , pp. 84 - 90
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

Allard, F., Hauschildt, P.H., 1995, ApJ 445, 433 Google Scholar
Alexander, D.R., Allard, F., Tamani, A., Hauschildt, P.H., 1997, Ap&SS 251, 171 Google Scholar
Aufdenberg, J.P., Hauschildt, P.H., Shore, S.N., 1998, ApJ 498, 837 Google Scholar
Burnashev, V.I., 1982, Izv. Krymskoi Astro. Obs. 65, 94 Google Scholar
Dominik, C., Sedlmayr, E., Gail, H.-P., 1993, A&A 277, 578 Google Scholar
Fluks, M.A., Plez, B., The, P.S., De Winter, D., Westerlund, B.E., Steenman, H.C., 1994, A&AS 105, 311 Google Scholar
Hauschildt, P.H., Allard, F., Baron, E., 1999, ApJ 512, 377 CrossRefGoogle Scholar
Hauschildt, P.H., Baron, E., 1998, J. Comp. App. Math., in press Google Scholar
Gustafsson, B., J⊘rgensen, U.G., 1994, A&A Rev. 6, 19 Google Scholar
MacConnell, D.J., Wing, R.F., Costa, E., 1992, AJ 104, 821 Google Scholar
Mathis, J.S., Rumpl, W., Nordsieck, K.H., 1977, ApJ 217,425 CrossRefGoogle Scholar
Ridgway, S.T., Joyce, R.R., White, N.M., Wing, R.F., 1980, ApJ 235, 126 Google Scholar
Silva, D.R., Cornell, M.E., 1992, ApJ 81, 865 Google Scholar
Smith, V.S., Lambert, D.L., 1990, ApJS 72, 387 Google Scholar
Tsuji, T., 1998, in The Carbon Star Phenomenon , ed. Wing, R.F., IAU Symp. 177, Kluwer Academic Publishers, in press Google Scholar