Introduction to Stellar Structure
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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...
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.
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.
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