Stability boundaries for massive stars in the sHR diagram

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