Star Cluster Evolution
A Computational Guide
1st Edition
Will be published approx. on 9. January 2030
Book
Hardback
300 pages
978-3-527-41096-5 (ISBN)
Description
Written by a bestselling author, this is a modern view of thedynamics and evolution of star clusters combined with thoroughcoverage of the computational techniques. Targeted, relativelysimple programs are used to demonstrate basic points of physics,whereby these programs may be linked to show how the combination ofphysical processes can lead to qualitatively new behavior. Inaddition, illustrative examples are provided for the novice. Moreadvanced readers may experiment with the various modules (or writetheir own), allowing them to quickly modify the physics withouthaving to make wholesale changes to the larger program. Moretechnical issues, such as advanced algorithms, hardwareacceleration, and high-performance parallel computing, arediscussed in a series of appendices, with sample softwarecompatible with the framework provided on a companion web site.This is a simplified and streamlined version of the authors' ownMUSE research environment, and is compatible with the additionalsoftware found on the MUSE web site.
Aimed primarily at graduate students and post-docs, this is equallyof interest to observers and researchers in related fields whomight wish to model specific systems or processes of interest.
Aimed primarily at graduate students and post-docs, this is equallyof interest to observers and researchers in related fields whomight wish to model specific systems or processes of interest.
More details
Language
English
Place of publication
Berlin
Germany
Publishing group
Wiley-VCH Verlag GmbH
Target group
College/higher education
Illustrations
60 s/w Abbildungen
Dimensions
Height: 240 mm
Width: 170 mm
ISBN-13
978-3-527-41096-5 (9783527410965)
Copyright in bibliographic data is held by Nielsen Book Services Limited or its licensors: all rights reserved.
Schweitzer Classification
Persons
Steve McMillan earned a BA in Mathematics from Cambridge University in 1977 and a Ph.D in Astronomy from Harvard in 1983. He joined the Physics Department at Drexel University in 1987 and is currently distinguished Professor of Physics at Drexel. His professional interests include numerical simulation of stars and stellar systems, development of high-performance software for star cluster simulations, and the analysis and visualization of complex datasets. He is also co-author of two best-selling introductory astronomy textbooks. Simon Portegies Zwart got his Ph.D at Utrecht University in 1996. He worked as a postdoctoral fellow at the University of Amsterdam, Tokyo University (Japan), MIT (USA), and in Amsterdam. He is now Professor of Computational Astrophysics at the Sterrewacht Leiden. In 2007 he received the "Pastoor Schmeits" Prize for the most outstanding young Dutch astronomer, and in 2009 he received the VICI award for his research on star clusters. His professional interests are high-performance computing and gravitational stellar dynamics, particularly in the context of the ecology of dense stellar systems.
Content
OVERVIEW Observations of Star Clusters - Open Clusters - Globular Clusters - Young Massive Clusters - Galactiv Nuclei Open Questions STELLAR DYNAMICS Models and Time Scales - Dynamicsl Time - Virial Equilibrium - Commen Density Profiles - Two-Body Relaxation Particle Potential Solvers - Direct Summation Codes - Tree Codes - Softening Particle Integration Schemes - Second- and Fourth-Order Methods - Time Step Algorithms External Fields The Stellar Mass Function Examples and Applications - Violent Relaxation - Mass Segregation - Core Collapse - Evaporation STELLAR EVOLUTION Modelling Stellar Evolution - Toy Models - Table Look-Up - Self-Consistent Stellar Evolution Codes Interfacing Stellar Evolution with Dynamics: The MUSE Modular Interface Examples and Applications - Mass Segregation with Stellar Evolution - Core Collapse with Stellar Evolution - Mass Loss and Cluster Lifetimes BINARY DYNAMICS Binary Properties - Dynamically Formed Binaries - "Primordial" Binaries Numerical Methods - Direct Integration - Regularization - Incorporation into the MUSE Framework Examples and Applications - Binary-Single Star Scattering; Heggie's Law - Binary-Binary Interactions - Binary Ejection and Destruction - Multiple Interactions - Binary Heating in Star Clusters BINARY EVOLUTION Physical Processes - Detached Evolution - Semi-Detached Evolution - Contact Evolution - Mergers Implementation in MUSE - Simplified Models - More Detailed Treatments Examples and Applications - Scattering Experiments: Punctated Binary Evolution - Population Synthesis with and without Dynamics STELLAR INTERACTIONS AND COLLISIONS Collisions and Mergers - Direct Interactions - Binary-Mediated Interactions - Mergers from Binary Evolution - Observational Consequences Modeling Stellar Mergers - Sticky Spheres - Entropy and Density Sorting Examples and Applications - Mergers and Mass Loss - Blue Stragglers - Low-Mass X-Ray Binaries MODELING DENSE STELLAR SYSTEMS Observations and Initial Conditions Early Cluster Evolution OB Dynamical Runaways Collision Runaways Black Hole Self-Ejection APPENDIX A: INITIAL CONDITIONS Stellar Mass Function Mass Segregation Virial Ratio Spatial Density and Velocity Distributions Tidal Field Binary Fraction Binary Secondary Masses Binary Orbital Elements Higher-Order Multiples APPENDIX B: COMMON DIAGNOSTICS Global Quantities - Total Mass and Energy - Virial Radius - Center of Mass - Density Center Lagrangian Radii Core Radius Density and Luminosity Profiles Stellar Mass and Luminosity Distributions - Total - By Percentile Velocity Dispersion and Anisotropy - Total - By Percentile Binary Properties - Total - By Percentile APPENDIX C: MUSE IMPLEMENTATION DETAILS The MUSE Software Framework Modular Structure Modules and Interfaces Sample Scripts APPENDIX D: HIGH-PERFORMANCE DYNAMICS Parallel Implementations The GRAPE Project Acceleration Using Graphics Processing Units