The diverse forms that stars assume in the course of their lives can all be derived from the initial conditions : the mass and the original chemical composition. In this textbook the basic concepts of stellar structure and the main roads of stellar evolution are described.
First, the observable parameters are presented, which are based on the radiation emerging from a stellar atmosphere. Then the basic physics is described, such as the physics of gases, radiation transport, and nuclear processes, followed by essential aspects of modelling the structure of stars. After a chapter on star formation, the various steps in the evolution of stars are presented. This leads us to brown dwarfs, to the way a star changes into the red-giant state and numerous other stages of evolution and ultimately to the stellar ashes such as white dwarfs, supernovae and neutron stars. Stellar winds, stellar rotation and convection all in? uence the way a star evolves. The evolution of binary stars is included by using several canonical examples in which interactive processes lead to X-ray binaries and supernovae of type Ia. Finally, the consequences of the study of stellar evolution are tied to observed mass and luminosity functions and to the overall evolution of matter in the universe.
The authors aim at reaching an understanding of stars and their evolution by both graduate students and astronomers who are not themselves investigating stars. To that end, numerous graphs and sketches, among which the Hertzsprung-Russell diagram is the dominant one, help trace the ways of stellar evolution. Ample references to specialised review articles as well as to relevant research papers are included.
L'auteur - Klaas De Boer
Klaas de Boer was born and educated in Groningen, the Netherlands. He specialized in optical and UV interstellar studies as well as in the UV output of old stars. After postdoctoral periods in Madison (WI, USA), Tübingen (Germany) and Herstmonceux (UK) he became professor at and Director of the Sternwarte of the University of Bonn. His main research interest is the three-dimensional structure of the local universe using stellar information.
L'auteur - Wilhelm Seggewiss
Wilhelm Seggewiss studied mathematics, physic and astronomy at the universities of München and Münster (Germany) where he got his PhD in astronomy. After postdoctoral assistantship at Münster he joined the staff of the observatory of the university of Bonn. After 1979 he became professor at Bonn and chairman of the observatory. Main fields of research are evolution of star cluster and the atmospheres of massive stars.
- Stellar atmosphere : continuum radiation + structure
- Stellar atmosphere : spectral structure
- Stellar atmosphere : basic equations
- Nuclear fusion in stars
- Stellar structure : making star models
- Star formation, proto-stars, very young stars
- The almost stars : Brown dwarfs
- Stars out of balance : from MS star to red giant
- Stellar evolution : stars in the lower mass range
- Stellar pulsation and vibration
- Stellar coronae, magnetic fields and sunspots
- Stellar evolution : stars in the higher mass range
- Rotation and stellar evolution
- The first stars
- Models and variation of "free" input parameters
- Degenerate stars : WD, NS, BH
- Evolution of binary stars
- Luminosity and mass function
- Stars influence their environment
- Summary; questions, constants, acronyms, lists
|Auteur(s)||Klaas De Boer, Wilhelm Seggewiss|
|Nb. de pages||314||333|
|Format||20 x 26||-|
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