Stellar Structure and Evolution (Astronomy and Astrophysics Library)
(Part of the Astronomy and Astrophysics Library Series)
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Book Overview
This long-awaited second edition of the classical textbook on Stellar Structure and Evolution by Kippenhahn and Weigert is a thoroughly revised version of the original text. Taking into account modern... This description may be from another edition of this product.
Format:Hardcover
Language:English
ISBN:3540502114
ISBN13:9783540502111
Release Date:July 1994
Publisher:Springer
Length:468 Pages
Weight:2.05 lbs.
Customer Reviews
3 ratings
Among astro texts...
Published by Thriftbooks.com User , 16 years ago
This text supports most every assertion with lengthy and invaluable derivations that are useful in ensuring that students understand the material. The topics are covered with exceptional depth, and the explanations are unusually readable. Compared with other astrophysics textbooks marketed to a similar audience, _Stellar Structure and Evolution_ is the sort of resource that will follow me through future courses, and although it was only recommended (rather than required) for my current class, I'm extremely glad I decided to purchase it.
very nice book
Published by Thriftbooks.com User , 17 years ago
very nice book, clear and good written. it permits me to pass the university exam, because the professor use it for his lessons. just to know that it italy this book costs over 150 euro!
A star's lifetime
Published by Thriftbooks.com User , 21 years ago
What happens in the lifetime of a star? This basically is the subject of the book. It describes from basic physical principles where ever possible how a star is formed and how it burns. Kippenhahn shows how inside a star, the gravitational pressure is necessarily balanced by the outgoing radiation and matter pressure. We see the cycle of how a star burns its hydrogen, synthesising helium in the process. Then, how heavier elements are formed. Finally, whether a star novas or not, depending on its mass. The Hertzsprung-Russell diagram is shown as a concise way to describe the lifecycle trajectory of a star, over billions of years. Well suited for physics students.
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