Item description for Stellar Structure and Evolution (Astronomy and Astrophysics Library) by Rudolf Kippenhahn...
This text gives a complete and comprehensive treatment of the physics of the stellar interior and the underlying fundamental processes and parameters. The models developed to explain the stability, dynamics and evolution of the stars are presented, and great care is taken to detail the various stages in a star's life. The authors have written a unique text based on their own pioneering work in stellar modeling. Since its publication, this textbook has come to be considered a classic by readers and teachers in astrophysics. This study edition is meant for students in astronomy and physics alike.
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Est. Packaging Dimensions: Length: 9.21" Width: 6.14" Height: 0.63" Weight: 1.54 lbs.
Release Date May 9, 1996
ISBN 3540580131 ISBN13 9783540580133
Availability 87 units. Availability accurate as of Oct 23, 2016 12:39.
Usually ships within one to two business days from La Vergne, TN.
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More About Rudolf Kippenhahn
Kippenhahn is Director of The Max Planck Institute for Astrophysics.
Rudolf Kippenhahn currently resides in Munich. Rudolf Kippenhahn was born in 1926.
Reviews - What do customers think about Stellar Structure and Evolution (Astronomy and Astrophysics Library)?
Pages coming off Aug 25, 2008
It arrived to me in Italy 20-15 days before the standard international shipping's time, in perfect conditions, as bought from the bookshop. Few days later the first page came off.
very nice book May 9, 2008
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 Jul 29, 2004
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.