Supernovae and Nucleosynthesis : : An Investigation of the History of Matter, from the Big Bang to the Present / / David Arnett.

• Superior document: Title is part of eBook package: De Gruyter Princeton University Press eBook-Package Archive 1927-1999
• VerfasserIn: Arnett, David,
• Place / Publishing House: Princeton, NJ : : Princeton University Press, , [2020]; ©1996
• Year of Publication: 2020
• Language: English
• Series: Princeton Series in Astrophysics ; 55
• Physical Description: 1 online resource (496 p.) :; 67 tables, 119 line drawings

This book investigates the question of how matter has evolved since its origin in the Big Bang, from the cosmological synthesis of hydrogen and helium to the generation of the complex set of nuclei that comprise our world and our selves. A central theme is the evolution of gravitationally contained...

Table of Contents

• Frontmatter
• Contents
• List of Figures
• List of Tables
• Preface
• 1 Introduction
• 2 Abundances of Nuclei
• Introduction
• 2.1 What Are Abundances?
• 2.2 Solar System Abundances
• 2.3 Stellar Atmospheres
• 2.4 Meteorites
• 2.5 Cosmic Rays
• 2.6 Other Aspects
• 3 Some Aspects of Nuclear Physics
• Introduction
• 3.1 Nuclear Masses
• 3.2 Nuclear Stability
• 3.3 Coulomb Barrier
• 3.4 Resonances
• 3.5 Reverse Rates
• 3.6 Heavy-Ion Reactions
• 3.7 Weak Interactions in Nuclei
• 3.8 Sources of Rates
• 4 Nuclear Reaction Networks
• Introduction
• 4.1 Network Equations
• 4.2 Solutions: Steady State
• 4.3 Solutions: Equilibria
• 4.4 Solutions: General Method
• 4.5 Energy Generation
• 4.6 Mixing and Hydrodynamics
• 4.7 Freezeout
• 5 Cosmological Nucleosynthesis
• Introduction
• 5.1 Kinematics
• 5.2 Radiation and Particles
• 5.3 Weak Interaction Freezeout
• 5.4 Cosmological Nucleosynthesis
• 5.5 Further Implications
• 6 Some Properties of Stars
• Introduction
• 6.1 Stellar Evolution Equations
• 6.2 Standard Model
• 6.3 Nuclear Energy
• 6.4 Neutrino Processes
• 6.5 Stellar Energy
• 6.6 Ignition Masses
• 6.7 Final States
• 7 Hydrogen-Burning Stars
• Introduction
• 7.1 Birth of Stars
• 7.2 Burning Processes
• 7.3 Main Sequence
• 7.4 Convective Cores
• 7.5 Shell Burning
• 7.6 Nucleosynthesis
• 8 Helium-Burning Stars
• Introduction
• 8.1 Thermonuclear Features
• 8.2 Ignition
• 8.3 Core Nucleosynthesis
• 8.4 Shell Nucleosynthesis
• 8.5 M-Ma Relation
• 8.6 Implications
• 9 Explosive Nucleosynthesis
• Introduction
• 9.1 Parameters
• 9.2 Carbon and Neon
• 9.3 Oxygen
• 9.4 Silicon and e-Process
• 9.5 Neutron Excess and Galactic Evolution
• 9.6 Yield Puzzle
• 10 Neutrino-Cooled Stars
• Introduction
• 10.1 Neutrinos and Convection
• 10.2 Core Evolution
• 10.3 Stellar Structure
• 10.4 Shell Nucleosynthesis
• 11 Thermonuclear Explosions
• Introduction
• 11.1 Thermonuclear Flames
• 11.2 Degenerate Instability
• 11.3 Convection and Urea
• 11.4 Yields from Degenerate Instability
• 11.5 He Detonation
• 11.6 Pair Instability
• 11.7 Oxygen Burning and Beyond
• 12 Gravitational Collapse
• Introduction
• 12.1 Historical Overview
• 12.2 Neutronization and Dissociation
• 12.3 Neutrino Trapping
• 12.4 Collapse
• 12.5 Bounce
• 12.6 Ejection of Matter
• 13 Supernovae
• Introduction
• 13.1 An Overview
• 13.2 Shock Emergence
• 13.3 Expansion and Radiative Diffusion
• 13.4 Radioactive Heating
• 13.5 Recombination
• 13.6 SN1987A
• 13.7 Type II Supernovae and SN1993J
• 13.8 Type I Supernovae
• 14 Galactic Evolution
• Introduction
• 14.1 Galactic Evolution Equations
• 14.2 Initial Mass Functions
• 14.3 One-Zone Models
• 14.4 Absolute Yields
• 14.5 The Galactic Disk
• 14.6 Primordial Stellar Yields
• 14.7 Critical Uncertainties
• Appendixes
• A. Solar System Abundances
• B. Equations of State
• C. Stellar Structure
• D. Supernova Light Curves
• References
• Index
• About the Author