Book contents
- Frontmatter
- Contents
- Preface
- Part I Introduction and overview
- Part II Basic physical processes in stellar interiors
- Part III Pre-main sequence, main sequence, and shell hydrogen-burning evolution of single stars
- 9 Star formation, pre-main sequence evolution, and the zero age main sequence
- 10 Solar structure and neutrino physics
- 11 Evolution through hydrogen-burning phases of models of mass 1, 5, and 25 M☉
- Index
- References
11 - Evolution through hydrogen-burning phases of models of mass 1, 5, and 25 M☉
from Part III - Pre-main sequence, main sequence, and shell hydrogen-burning evolution of single stars
Published online by Cambridge University Press: 05 December 2012
- Frontmatter
- Contents
- Preface
- Part I Introduction and overview
- Part II Basic physical processes in stellar interiors
- Part III Pre-main sequence, main sequence, and shell hydrogen-burning evolution of single stars
- 9 Star formation, pre-main sequence evolution, and the zero age main sequence
- 10 Solar structure and neutrino physics
- 11 Evolution through hydrogen-burning phases of models of mass 1, 5, and 25 M☉
- Index
- References
Summary
In this chapter,models ofmass 1, 5, and 25 M☉ and of population I composition (Z = 0.015 and Y = 0.275) are evolved through all phases of hydrogen burning up to the point when helium is ignited in a hydrogen-exhausted core. The model masses have been chosen with the aim of representing three broad classes of stars. Models of mass less than 0.5 M☉ have been excluded from consideration not only because they evolve on a time scale much longer than a Hubble time, but, because they remain completely convective throughout their nuclear burning lives, they can be described adequately by a sequence of polytropes, as discussed in Section 5.6, without invoking the elaboration of an evolutionary calculation. The 1 M☉ model is representative of a class of stars which evolve in less than a Hubble time into red giants with an electron-degenerate helium core and ignite helium in a semiexplosive fashion. These stars, of mass extending to ˜2.25 M☉, eventually become AGB stars with a carbon-oxygen core and, after ejecting a nebular shell, evolve into CO white dwarfs of mass ˜0.55 M☉ The 5 M☉ model is representative of stars in the approximate mass range 2.25 <M/M☉ <10.5 which ignite helium under non electron-degenerate conditions, but during and following the quiescent helium-burning phase evolve in a fashion similar to the evolution of lower mass stars during and after the quiescent helium-burning phase.
- Type
- Chapter
- Information
- Stellar Evolution Physics , pp. 714 - 845Publisher: Cambridge University PressPrint publication year: 2012