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Stability boundaries for massive stars in the sHR diagram

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Abstract

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 $4\log T_{\rm eff}-\log g \,(= \log L/M)$. 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.

Citation

(2015). Stability boundaries for massive stars in the sHR diagram. Proceedings of the International Astronomical Union, 230-231. https://doi.org/10.1017/S1743921314006838

Acceptance Date Jan 23, 2015
Publication Date Jan 23, 2015
Journal Proceedings of the International Astronomical Union
Print ISSN 1743-9213
Publisher Cambridge University Press
Pages 230-231
DOI https://doi.org/10.1017/S1743921314006838
Keywords stars, evolution, oscillations, mass loss, Hertzsprung-Russell diagram
Publisher URL http://doi.org/10.1017/S1743921314006838

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