Stability boundaries for massive stars in the sHR diagram

Hideyuki Saio; Cyril Georgy; Georges Meynet

doi:10.1017/S1743921314006838

Stability boundaries for massive stars in the sHR diagram

Hideyuki Saio, Cyril Georgy, Georges Meynet

Science

Research output: Contribution to journal › Article › peer-review

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 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.

Original language	English
Pages (from-to)	230-231
Number of pages	2
Journal	Proceedings of the International Astronomical Union
Volume	9
DOIs	https://doi.org/10.1017/S1743921314006838
Publication status	Published - 2014

Keywords

Hertzsprung-Russell diagram
stars: evolution
stars: mass loss
stars: oscillations

ASJC Scopus subject areas

Medicine (miscellaneous)
Astronomy and Astrophysics
Nutrition and Dietetics
Public Health, Environmental and Occupational Health
Space and Planetary Science

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title = "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 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.",

keywords = "Hertzsprung-Russell diagram, stars: evolution, stars: mass loss, stars: oscillations",

author = "Hideyuki Saio and Cyril Georgy and Georges Meynet",

year = "2014",

doi = "10.1017/S1743921314006838",

language = "English",

volume = "9",

pages = "230--231",

journal = "Proceedings of the International Astronomical Union",

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T1 - Stability boundaries for massive stars in the sHR diagram

AU - Saio, Hideyuki

AU - Georgy, Cyril

AU - Meynet, Georges

PY - 2014

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N2 - 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 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.

AB - 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 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.

KW - Hertzsprung-Russell diagram

KW - stars: evolution

KW - stars: mass loss

KW - stars: oscillations

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