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The Spheroidal/Ellipsoidal, Variable Mass-Loss, Decelerated Be Star Model (Review Paper)

Published online by Cambridge University Press:  23 September 2016

V. Doazan

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The proposed model is empirical; it is based on analysis of the available data on Be stars obtained in all the observable spectral regions, and it is required to be thermodynamically self-consistent. Rather than trying to answer the question: “What is the origin of the Be-phenomenon?” We ask: First. “What phenomena characterize empirically Be stars?” Second, “What thermodynamic characteristics are implied by the existence of such phenomena?” Third. “What inferences may be made an the atmospheric structure of a Be star from these empirical and thermodynamical characteristics?” The observed phenomena, their thermodynamical implications and the resulting model have each two aspects. On the one hand, the observational evidence for a nonradiatively heated, expanding chromosphere-corona implies the existence of both a nonradiative energy flux and a mass outflow from the photosphere. This first aspect is common to both Be and normal B stars, at least for the earliest subtypes.

Type
IV. Models
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 384 - 410
Copyright
Copyright © Cambridge University Press 1987

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