Structure Formation in the Universe

Häftad, Engelska, 1993

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Beskrivning

Understanding the way in which large-scale structures like galaxies form remains the most challenging problem in cosmology today. This text provides an up-to-date and pedagogical introduction to this exciting area of research. Part 1 deals with the Friedmann model, the thermal history of the Universe, and includes a description of observed structures in the Universe. Part 2 describes the theory of gravitational instability in both the linear and non-linear regimes. This part also includes chapters on the microwave background radiation, large-scale velocity fields, quasars and high redshift objects. Part 3 covers inflation, cosmic strings and dark matter. Each chapter is accompanied by a comprehensive set of exercises to help the reader in self-study. The book will be of interest to research and graduate students in cosmology, relativity, theoretical physics, astrophysics and astronomy. It is also suitable for use as a graduate textbook for introductory graduate level courses.

Produktinformation

Utgivningsdatum:1993-05-06
Mått:181 x 255 x 31 mm
Vikt:865 g
Format:Häftad
Språk:Engelska
Antal sidor:500
Förlag:Cambridge University Press
ISBN:9780521424868

Utforska kategorier

Fysik inom Naturvetenskap och teknik

Recensioner i media

'Padmanabhan has written an invaluable exposition from first physical principles of almost all the things that a new graduate student embarking upon research in theoretical cosmology needs to know … A unique feature, for a book at this level, is the extensive collection of advanced problems at the end of each chapter … Overall, I found Padmanabhan's book to be an extremely useful working text that covers most of the topics at the research frontier.' Prof. John Barrow, The Times Higher Education Supplement

Innehållsförteckning

Preface; Part I. The Smooth Universe: 1. Introducing the Universe; 2. The Friedmann model; 3. Thermal history of the Universe; Part II. The Clumpy Universe: 4. Growth of linear perturbations; 5. Statistical properties of the density fluctuations; 6. The microwave background radiation; 7. The linear theory: velocity fields; 8. The non-linear evolution; 9. The non-linear theory: high redshift objects; Part III. Towards a More Complete Picture: 10. The origin of initial perturbations; 11. Dark matter; 12. Epilogue; Appendices; Notes and references; Index.