Titlebook: Late Stages of Stellar Evolution; R. J. Tayler,J. E. Hesser Book 1974 International Astronomical Union 1974 gravitation.gravity.planet.sta

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R. J. Tayler,J. E. Hessertochemistry,histologicalstaining (Chapters10and11),aswellasspecificmethods for the in situ identification of hypoxia (Chapter 12) and apoptosis (Chapter 13). Finally, Part III details advances in imaging (Chapt978-1-4939-5694-4978-1-60327-345-9Series ISSN 1064-3745 Series E-ISSN 1940-6029

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Mass Ejection by Radiation Pressure, the optically thick regions. There were many attempts to find selfconsistent models of time-independent mass outflow driven by this mechanism (Finzi and Wolf, 1971; Bisnovaty-Kogan and Nadyozhin, 1972; and many others); however, neither was satisfactory.

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,Evolution of Stars with , ≤ 8,,,f such stars, ., are below .. = 8 .. ± ± 2 ... The low mass stars (..) lose their envelopes and become white dwarfs. The intermediate stars (.. < ..) ignite carbon in their highly degenerate cores of 1.4 ... Present observational and/or theoretical estimates of .. are very uncertain. Problems associ

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,Evolution of Stars with , ≥ 8 ,,,he helium-burning stage provides evidence for the existence of neutrino emission predicted by the theory of universal Fermi-interaction. The criterion for convective stability in the zone of variable molecular weight still remains uncertain despite several possibilities for a unique choice of the st

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Stability Properties of Stars with Central He Burning,static (.. = 0) solutions with the same chemical profile sometimes exist for such stars when . ? 9 .. (Lauterborn .., 1971; Kozlowski, 1971). Which of these solutions the corresponding evolutionary models will choose depends on the evolutionary history of the star. Stability properties of such stars

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