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Stability boundaries for massive stars in the sHR diagram

Published online by Cambridge University Press:  23 January 2015

Hideyuki Saio ,
Cyril Georgy  and
Georges Meynet
Hideyuki Saio
Affiliation:
Tohoku University, Japan email: saio@astr.tohoku.ac.jp
Cyril Georgy
Affiliation:
Keele University, UK
Georges Meynet
Affiliation:
Geneva observatory, Switzerland
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Abstract

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Stability boundaries of radial pulsations in massive stars are compared with positions of variable and non-variable blue-supergiants in the spectroscopic HR (sHR) diagram (Langer & Kudritzki 2014), whose vertical axis is 4 log Teff - log g(= log L/M). Observational data indicate that variables tend to have higher L/M than non-variables in agreement with the theoretical prediction. However, many variable blue-supergiants are found to have values of L/M below the theoretical stability boundary; i.e., surface gravities seem to be too high by around 0.2-0.3 dex.

Keywords

stars: evolutionstars: oscillationsstars: mass lossHertzsprung-Russell diagram
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 230 - 231
Copyright
Copyright © International Astronomical Union 2015 

References

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