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The Carbon Stars Adventure

Modelling C-star atmospheres†

Published online by Cambridge University Press:  27 October 2016

Gioia Rau ,
C. Paladini ,
J. Hron ,
B. Aringer ,
K. Eriksson ,
M. A. T. Groenewegen  and
W. Nowotny
Gioia Rau
Affiliation:
University of Vienna, Department of Astrophysics, Türkenschanzstrasse 17, A-1180 Vienna email: gioia.rau@univie.ac.at
C. Paladini
Affiliation:
Institut d'Astronomie et d'Astrophysique, Universite' libre de Bruxelles, Belgium
J. Hron
Affiliation:
University of Vienna, Department of Astrophysics, Türkenschanzstrasse 17, A-1180 Vienna email: gioia.rau@univie.ac.at
B. Aringer
Affiliation:
Department of Physics and Astronomy G. Galilei, Padova, Italy
K. Eriksson
Affiliation:
Department of Physics and Astronomy, Uppsala University
M. A. T. Groenewegen
Affiliation:
Royal Observatory of Belgium, Belgium
W. Nowotny
Affiliation:
University of Vienna, Department of Astrophysics, Türkenschanzstrasse 17, A-1180 Vienna email: gioia.rau@univie.ac.at
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Abstract

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We compare in a systematic way spectrometric, photometric and mid-infrared (VLTI/MIDI) interferometric measurements with different types of model atmospheres. Self-consistent dynamic model atmospheres in particular were used to interpret in a consistent way the dynamic behavior of gas and dust. The results underline how the joint use of different kind of observations, as photometry, spectroscopy and interferometry, is essential to understand the atmospheres of pulsating C-rich AGB stars. The sample of C-rich stars discussed in this work provides crucial constraints for the atmospheric structure.

Keywords

instrumentation: high angular resolutiontechniques: interferometricstars: AGB and post-AGBstars: atmospheresstars: circumstellar matterstars: fundamental parameters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 160 - 161
Copyright
Copyright © International Astronomical Union 2016 

Footnotes

†

This work is supported by the Austrian Science Fund FWF under project number P23006-N16.

References

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