Titlebook: Structure and Evolution of Single and Binary Stars; C. W. H. Loore,C. Doom Book 1992 Springer Science+Business Media New York 1992 star.st

洞穴

Nuclear Burning in Stellar Interiors,We say that the (compound) nucleus is not thermalized before interacting again. An example of such a reaction is :.The compound nucleus of .Al does not decay to its ground state but transforms into .Mg through a beta decay.

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obligation

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The Evolution of Low and Intermediate Mass Binary Systems,y considered as circular. The rotation of the components is assumed to be synchronized with the orbital motion. The evolution of close binary systems depends on the masses of the components, the mass ratio and the orbital period.

Terminal

acheon

Incommensurate

The Evolution of Massive Close Binaries,ell as for massive close binaries, phases of mass exchange can occur during core hydrogen burning, shell hydrogen burning and helium burning. For massive close binaries mass loss by stellar wind already changes the orbital elements (see Chapter 15, eq. 15.34).

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永久

The Evolution of Binary Stars General Considerations,ass and angular momentum transfer may occur, these three parameters will change during the evolution. We may distinguish between unevolved systems (before possible interaction between the components) and evolved systems.

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Book 1992ure and evolution including achapter on numerical modelling. The second part deals with specificevolutionary aspects of single and binary stars with a variety ofmasses. The last chapter gives several models of stars with specificmasses. .The book is intended as an introduction for students, as well as areference for researchers.