Buch, Englisch, 356 Seiten, Format (B × H): 155 mm x 235 mm, Gewicht: 540 g
Buch, Englisch, 356 Seiten, Format (B × H): 155 mm x 235 mm, Gewicht: 540 g
Reihe: Astrophysics and Space Science Library
ISBN: 978-1-4020-0376-9
Verlag: Springer
The evolution of galaxies is governed mainly by the evolution of massive stars whereas the evolution of a massive star depends primarily on its mass, chemical composition and on whether or not the star is a Single object or a binary component. To study the evolution of galaxies, it is therefore essential to know how stellar masses are distributed at birth, how many stars are formed in binaries, and what the mass ratio and orbital period distribution of binaries look like. Massive stars are intrinsically the brightest stars, so that it may be possible to discover their properties in distant groups prOvided that large telescopes can be used for basic stellar observations. However, until now the observations of massive stars have been reasonably complete only for a small region of our own Galaxy (~ 3 kpc from the Sun). One hopes that the conclusions resulting from these observations hold for the whole Galaxy, for the whole cosmos. With 'The Brightest Stars' of De Jager (1980) in mind, the present monograph is an addendum and an update in which we discuss the observations of 'The Brightest Binaries' in the framework of stellar evolution. A small or intermediate mass star close to the Sun may look brighter than a massive one far away. However, within volume limited star samples, the massive stars are on average also the brightest ones. In the present monograph (similarly as in the work of De Jager), bright means massive. The book consists of four main chapters.
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List of abbreviations.- Constants.- I: Massive Stars.- 1. Definition.- 2. General observations.- II: Massive Single Stars.- 3. The equations of stellar structure of a non-magnetic, non-rotating single star.- 4. Evolutionary computations of non-rotating massive single stars.- 5. Comparison between observations and evolutionary computations of non-rotating single stars.- 6. The effect of rotation on the evolution of massive single stars.- III: Massive Close Binaries.- 7. General.- 8. The Roche model.- 9. The mass transfer process during RLOF.- 10. The evolution of the binary period in MCBs.- 11. The effect of the supernova explosion of one of the components.- 12. Evolutionary computations of massive close binaries.- 13. Massive binaries: observations.- 14. Comparison between the predicted evolution of MCBs and observations.- IV: Massive Star Population Number Synthesis.- 15. General.- 16. Observations used as input in a population model.- 17. The observations which need to be reproduced by a massive star population model.- 18. The population number synthesis (PNS) model.- 19. PNS model calculations.- Concluding remarks.- References.
