Introduction to stellar structure
Material type:
TextLanguage: English Publication details: Switzerland: Springer, 2016.Description: xv, 215p. : illISBN: - 9783319161419
- C:(B96) Q6 TC
Textbook
| Cover image | Item type | Current library | Home library | Collection | Shelving location | Call number | Materials specified | Vol info | URL | Copy number | Status | Notes | Date due | Barcode | Item holds | Item hold queue priority | Course reserves | |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
Textbook
|
Central Science Library | Central Science Library | C:(B96) Q6 TC (Browse shelf(Opens below)) | Available | SL1601242 |
Browsing Central Science Library shelves Close shelf browser (Hides shelf browser)
|
|
|
|
No cover image available No cover image available | No cover image available No cover image available | No cover image available No cover image available | ||
| C:(B28) R2 Physics of datd science and machine learning | C:(B280b9S) Q3 TC Statistical data analysis for the physical sciences | C:(B316) Q3 TC Knots and physics | C:(B96) Q6 TC Introduction to stellar structure | Cc3:m74 H6 Cavendush laboratory | Cc73.M86 G9 Demonstration laboratory of physics at the university of Chicago | CcB3,7:35 L2.2 Dynamic mass spectrometry |
Index 211-215p.
This book provides a comprehensive overview of stellar structure, evolution and basic stellar properties. It includes integrated problems within the chapters, with worked solutions.
In the first part of this book, the author presents the basic properties of the stellar interior and describes them thoroughly, along with deriving the main stellar structure equations of temperature, density, pressure and luminosity, among others. The process and application of solving these equations is explained, as well as linking these results with actual observations. The second part of the text describes what happens to a star over time and how to determine this by solving the same equations at different points during a star’s lifetime. The fate of various stars is quite different depending on their masses and this is described in the final parts of the book. This text can be used for an upper level undergraduate course or an introductory graduate course on stellar physics.
There are no comments on this title.
