Anmerkung: Intro -- Foreword -- Preface -- Contents -- List of Figures -- List of Tables -- Part ITheory of Star Formation and DynamicalEvolution of Stellar Systems -- 1 The Raw Material of Cluster Formation: Observational Constraints -- 1.1 Overview of Molecular Cloud Observations -- 1.2 Observational Techniques Applied to GMCs -- 1.2.1 Molecular Line Emission -- 1.2.2 Dust Emission -- 1.2.3 Dust Absorption -- 1.3 Magnetic Support and the Star Formation Efficiency Problem -- 1.4 Scaling Relations -- 1.5 GMCs and the Large-Scale ISM -- 1.6 Summary: Key Observational Constraints for Simulations -- References -- 2 The Numerical Tools for Star Cluster Formation Simulations -- 2.1 The Pure Gravitational Problem -- 2.2 Hydrodynamical Problems: A Quick Guide to SPH -- 2.3 Adding `More Physics' to Hydrodynamical Codes -- 2.4 Summary -- References -- 3 The Comparison of Observational and Simulation Data -- 3.1 The Characterisation of Observational and Simulated Data -- 3.1.1 Characterising Gaseous Structures -- 3.1.2 Characterising Stellar Distributions -- 3.1.3 Characterising the IMF -- 3.2 Simulation Results: Bonnell et al. (2008) as a Case Study -- 3.3 The Relationship Between Gas, Cores and Stars in Simulations -- 3.4 The Origin of the Stellar IMF in `Vanilla' Calculations -- 3.5 Summary -- References -- 4 The Role of Feedback and Magnetic Fields -- 4.1 Varying the Parameters -- 4.2 Putting in More Physics -- 4.2.1 Thermal Feedback -- 4.2.2 Outflows -- 4.2.3 Magnetic Fields -- 4.2.4 Ionising Radiation -- 4.3 Discussion -- 4.4 Summary -- References -- 5 The Formation of Multiple Systems in Clusters -- 5.1 The Formation of Multiple Stars in `Vanilla' Simulations -- 5.1.1 Binary Star Statistics -- 5.1.2 Disc Orientation in Protobinaries -- 5.1.3 Predictions for Higher-Order Multiples -- 5.2 The Effect of `Additional Physics' on Multiple Star Formation. , 5.3 Summary -- References -- 6 The Role of N-body Dynamics in Early Cluster Evolution -- 6.1 Mass Segregation -- 6.2 The Destruction of Binaries in Clusters -- 6.3 Stellar Dynamics Plus Gas: Stellar Collisions -- 6.4 Stellar Dynamics with Gas Removal: Infant Mortality -- 6.5 Summary -- References -- 7 Concluding Issues -- 7.1 Modelling Individual Clusters -- 7.1.1 Gas-Free Studies -- 7.1.2 Embedded Star-Forming Regions -- 7.2 Imprint of Cluster Origin on Field Star Populations -- 7.3 Imprint of Cluster Birthplace on Discs -- 7.4 The Birth Environment of the Sun -- 7.5 Summary -- References -- Part IIKinematics of Star Clustersand Associations -- 8 Introduction to Open Clusters -- 8.1 Introduction -- 8.2 Classical Open Clusters -- 8.2.1 Definition -- 8.2.2 Global Properties -- 8.2.3 Internal Properties -- 8.2.4 OB Associations -- 8.3 Closing Thought -- References -- 9 Overview of Multiple Star Systems -- 9.1 Introduction -- 9.2 Field Solar-Type Binary Population -- 9.3 Field OB Binary Population -- 9.4 Open Cluster Solar-Type Binary Population -- 9.5 Closing Thoughts -- References -- 10 Overview of Collisional Stellar Dynamics -- 10.1 Introduction -- 10.2 Timescales -- 10.3 Violent Relaxation -- 10.4 Energy Equipartition and Mass Segregation -- 10.5 Evolution of Dynamical Systems: Some Fundamental Physics -- 10.6 Evolution of Dynamical Systems: Two-Body Processes -- 10.7 Evolution of Dynamical Systems: Cluster Dissolution -- References -- 11 λ Ori: A Case Study in Star Formation -- 11.1 Introduction -- 11.2 Overview -- 11.3 Dust and Molecular Gas -- 11.4 Massive Stars -- 11.5 Low-Mass Stars -- 11.5.1 Hα Emission and Objective Prism Surveys -- 11.5.2 Lithium Absorption and Multi-Object Spectroscopic Surveys -- 11.5.3 Photometric Surveys -- 11.6 Analysis of a Star-Forming Region -- 11.6.1 Distance -- 11.6.2 Spatial Distribution of Star Formation. , 11.6.3 Initial Mass Function -- 11.6.4 Total Stellar Population -- 11.6.5 Accretion Disc Evolution -- 11.6.6 Age Distribution -- 11.7 The Star Formation History of λ Ori -- 11.8 Final Thought -- References -- 12 Overview of Star-Forming Regions -- 12.1 Introduction -- 12.2 Taurus-Auriga -- 12.3 Orion Molecular Cloud -- 12.4 Young Embedded Clusters -- References -- 13 Kinematics of Star-Forming Regions -- 13.1 Introduction -- 13.2 OB Associations After Hipparcos -- 13.3 Kinematics in Star-Forming Associations -- 13.4 Stellar Kinematics in Young Star Clusters -- References -- 14 Pre-main-sequence Binaries -- 14.1 Introduction -- 14.2 Pre-main-sequence Binary Frequency -- 14.2.1 Definition -- 14.2.2 Frequency as a Function of Star-Forming Region -- 14.2.3 Frequency as a Function of Orbital Period -- 14.2.4 Higher-Order Multiplicity -- 14.2.5 Protobinaries -- 14.3 Pre-main-sequence Binaries and Disc Evolution -- 14.4 Concluding Thought -- References -- Part IIIFrom Whence the Field? -- 15 Galactic Demographics: Setting the Scene -- 15.1 Introduction -- 15.2 The Nature of the Milky Way -- 15.3 The Milky Way as a Galaxy: Large-Scale Properties -- 15.4 Star Formation in the Milky Way -- 15.5 Stellar Abundances -- 15.6 The Sun's Place in the Milky Way -- References -- 16 The Solar Neighbourhood -- 16.1 Introduction: Act Locally, Think Globally -- 16.2 The Local Volume and Local Samples -- 16.3 The Stellar Luminosity Function -- 16.4 Stellar Multiplicity -- 16.5 The Stellar Mass Function: Present Day and Initial -- 16.6 Is There a Universal IMF? -- 16.7 Summary -- References -- 17 Stellar Kinematics and the Dynamical Evolution of the Disc -- 17.1 Introduction -- 17.2 Building Stellar Kinematics as a Discipline -- 17.3 Kinematics of Local Stars -- 17.4 Star Streams and Moving Groups -- 17.5 Stellar Migration, Radial Mixing and the Galactic Bar -- 17.6 Summary. , References -- 18 Clusters and the Galactic Halo -- 18.1 Introduction -- 18.2 Globular Clusters and the Galactic Halo -- 18.3 Setting the Context -- 18.4 The ELS Model -- 18.5 Searle and Zinn and Galaxy Mergers -- 18.6 Globular Clusters Revisited -- 18.7 Endword -- References -- 19 Star Formation over Time -- 19.1 Introduction -- 19.2 The Structure of the Disc -- 19.3 Measuring Stellar Ages -- 19.3.1 Ages for Stars in Clusters -- 19.3.2 Ages for Individual Stars -- 19.4 The Age-Metallicity Relation and the Age Distribution of Local Stars -- 19.4.1 Stellar Metallicities -- 19.4.2 The Age-Metallicity Relation -- 19.4.3 The Age Distribution in the Disc -- 19.5 Summary -- References -- 20 Where Do Stars Form? -- 20.1 Introduction -- 20.2 OB Associations -- 20.3 The Taurus-Auriga Cloud -- 20.4 Young Stars Near the Sun -- 20.5 Clustered Star Formation: Open and Embedded Clusters -- 20.5.1 Open Clusters -- 20.5.2 Infrared Astronomy and the Detection of Embedded Clusters -- 20.5.3 Statistics of Embedded Clusters -- 20.6 Summary and Future Prospects -- References -- 21 Where Was the Sun Born? -- 21.1 Introduction -- 21.2 The Age of the Sun -- 21.3 The Sun's Chemical Composition -- 21.4 The Characteristics of the Solar System -- 21.5 The Sun's Natal Environment -- 21.6 Can We Find the Sun's Companions? -- 21.7 Summary and Conclusions -- References.

Anmerkung: Intro -- Preface -- Acknowledgements -- Contents -- List of Figures -- List of Tables -- 1 Physical Processes in Protoplanetary Disks -- 1.1 Preamble -- 1.2 Observational Context -- 1.2.1 The Classification of Young Stellar Objects -- 1.2.2 Accretion Rates and Lifetimes -- 1.2.3 Inferences from the Dust Continuum -- 1.2.4 Molecular Line Observations -- 1.2.5 Large-Scale-Structure in Disks -- 1.3 Disk Structure -- 1.3.1 Vertical and Radial Structure -- 1.3.2 Thermal Physics -- 1.3.3 Ionization Structure -- 1.4 Disk Evolution -- 1.4.1 The Classical Equations -- 1.4.2 Boundary Conditions -- 1.4.3 Viscous Heating -- 1.4.4 Warped Disks -- 1.4.5 Disk Winds -- 1.5 Turbulence -- 1.5.1 Hydrodynamic Turbulence -- 1.5.2 Self-gravity -- 1.5.3 Magnetohydrodynamic Turbulence and Transport -- 1.5.4 The Magnetorotational Instability -- 1.5.5 Transport in the Boundary Layer -- 1.6 Episodic Accretion -- 1.6.1 Secular Disk Instabilities -- 1.6.2 Triggered Accretion Outbursts -- 1.7 Single and Collective Particle Evolution -- 1.7.1 Radial Drift -- 1.7.2 Vertical Settling -- 1.7.3 Streaming Instability -- 1.8 Structure Formation in Protoplanetary Disks -- 1.8.1 Ice Lines -- 1.8.2 Particle Traps -- 1.8.3 Zonal Flows -- 1.8.4 Vortices -- 1.8.5 Rossby Wave Instability -- 1.9 Disk Dispersal -- 1.9.1 Photoevaporation -- 1.9.2 MHD Winds -- References -- 2 Planet Formation and Disk-Planet Interactions -- 2.1 Introduction -- 2.1.1 The Solar System -- 2.1.2 Properties of the Extrasolar Planets -- 2.1.3 Pathways to Planets -- 2.2 From Dust to Planetesimals -- 2.2.1 Study the Initial Growth Phase -- 2.2.2 How to Overcome Growth Barriers -- 2.2.3 Dust Concentration -- 2.3 Terrestrial Planet Formation -- 2.3.1 Concepts -- 2.3.2 Growth to Protoplanets -- 2.3.3 Assembly of the Terrestrial Planets -- 2.4 The Formation of Massive Planets by Core Accretion -- 2.4.1 Background. , 2.4.2 The Growth to a Giant -- 2.4.3 The Final Mass -- 2.4.4 Interior Structure of Planets -- 2.5 Planets Formed by Gravitational Instability -- 2.5.1 Background -- 2.5.2 Linear Stability Analyses -- 2.5.3 Fragmentation Conditions -- 2.5.4 Non-linear Simulations -- 2.6 Planet-Disk Interaction -- 2.6.1 Basic Concepts -- 2.6.2 Type I Migration -- 2.6.3 Type II Migration -- 2.6.4 Other Regimes of Migration -- 2.6.5 Eccentricity and Inclination -- 2.7 Multi-body Systems -- 2.7.1 Resonances -- 2.7.2 Dynamics -- 2.7.3 Multi-planet Systems -- 2.7.4 Circumbinary Planets -- References.

Anmerkung: Kiel, Univ., Diplomarbeit, 1975

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