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