The Gravitational Million–Body Problem
A Multidisciplinary Approach to Star Cluster Dynamics

A 2003 graduate text describing the theory astronomers need for studying globular star clusters.

Douglas Heggie (Author), Piet Hut (Author)

9780521774864, Cambridge University Press

Paperback, published 23 January 2003

372 pages, 85 b/w illus. 5 tables 136 exercises
24.7 x 17.4 x 2 cm, 0.793 kg

'What they did, covers many aspects of the problem: a historical overview, analytical details for the solvable cases, numerical solutions including computer codes for others, applications for astrophysical examples like star clusters, and a reference list covering twenty pages.' Zentralblatt MATH

The globular star clusters of the Milky Way contain hundreds of thousands of stars held together by gravitational interactions, and date from the time when the Milky Way was forming. This 2003 text describes the theory astronomers need for studying globular star clusters. The gravitational million-body problem is an idealised model for understanding the dynamics of a cluster with a million stars. After introducing the million-body problem from various view-points, the book systematically develops the tools needed for studying the million-body problems in nature, and introduces the most important theoretical models. Including a comprehensive treatment of few-body interactions, and developing an intuitive but quantitative understanding of the three-body problem, the book introduces numerical methods, relevant software, and current problems. Suitable for graduate students and researchers in astrophysics and astronomy, this text also has important applications in the fields of theoretical physics, computational science and mathematics.

Part I. Introductions: 1. Astrophysics introduction
2. Theoretical physics introduction
3. Computational physics introduction
4. Mathematical introduction
Part II. The Continuum Limit: 5. Paradoxical thermodynamics
6. Statistical mechanics
7. Motion in a central potential
8. Some famous models
9. Methods
Part III. Mean Field Dynamics: 10. Violent relaxation
11. Internal mass loss
12. External influences
Part IV. Microphysics: 13. Exponential orbit instability
14. Two-body relaxation
15. From Kepler to Kustaanheimo
Part V. Gravothermodynamics: 16. Escape and mass segregation
17. Gravothermal instability
18. Core collapse rate for star clusters
Part VI. Gravitational Scattering: 19. Thought experiments
20. Mathematical three-body scattering
21. Analytical approximations
22. Laboratory experiments
23. Gravitational burning and transmutation
Part VII. Primordial Binaries: 24. Binaries in star clusters
25. Triple formation and evolution
26. A non-renewable energy source
Part VIII. Post-Collapse Evolution: 27. Surviving core collapse
28. Gravothermal oscillations
29. Dissolution
Part IX. Star Cluster Ecology: 30. Stellar and dynamical evolution
31. Collisions and capture
32. Binary star evolution and blue stragglers
33. Star cluster evolution
Appendices.

Subject Areas: Astrophysics [PHVB]