Other
Scientific paper
May 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...426l..43s&link_type=abstract
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 426, no. 1, p. L43-L46
Other
30
Blue Stars, Hertzsprung-Russell Diagram, Magnetohydrodynamic Stability, Metallicity, Stellar Composition, Stellar Envelopes, Stellar Evolution, Stellar Luminosity, Stellar Mass Ejection, Stellar Models, Stellar Winds, Supergiant Stars, Variable Stars, Mathematical Models, Opacity, Stellar Mass, Stellar Temperature
Scientific paper
Two phases of dynamical instability are theoretically predicted to exist during the evolution of supergiants of normal metallicity that are initially more massive than approximately 60 solar mass. One phase occurs briefly in the yellow or red region of the Hertzsprung-Russell diagram for stars in the early stages of core helium burning, and the other phase occurs for a longer time in the blue or blue-white region for stars exhausting their core helium. Probably only the second phase exists in the case of supergiants with initial masses between approximately 60 solar mass and approximately 30 solar mass or with low metallicities The cause of instability is the partial ionization of hydrogen and helium in a quasi-isolated outer region of the stellar envelope, above the layer where the iron opacity attains a large local maximum. Predicted luminosities, effective temperatures, ejected nebular masses, remnant masses, eruption recurrence times, and lifetimes, though very approximate, are generally consistent with available observational data for the important class of unstable supergiants known as luminous blue variables.
Chin Chao-Wen
Stothers Richard B.
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