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

Condescending

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

compel

Outspoken

MOAN

Ancestor

homeostasis

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.

staging

,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

machination

neologism

,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

Perineum

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