Supernovae, Neutron Star Physics and Nucleosynthesis (Astronomy and Astrophysics Library)

This book deals with the interdisciplinary areas of nuclear physics, supernovae and neutron star physics. It addresses the physics and astrophysics of the spectacular supernova explosions, starting with the collapse of massive stars and ending with the birth of neutron stars or black holes. Recent progress in the understanding of core collapse supernova (CCSN) and observational aspects of future detections of neutrinos from CCSN explosions are discussed. The other main focus in this text is the novel phases of dense nuclear matter, its compositions and equation of state (EoS) from low to very high baryon density relevant to supernovae and neutron stars. The multi-messenger astrophysics of binary neutron star merger GW170817 and its relation to EoS through tidal deformability are also presented in detail. The synthesis of elements heavier than iron in the supernova and neutron star environment by the rapid (r)-process are treated here with special emphasis on the nucleosynthesis in the ejected material from GW170817. This monograph is written for graduate students and researchers in the field of nuclear astrophysics. Foreword Preface Contents Acronyms 1 Introduction 2 Theory of Supernova Explosions 2.1 Overview: Historical 2.2 Supernova Type Ia 2.3 Gravitational Collapse and Pre-supernova Conditions 2.4 Production of Neutrinos and Their Emission 2.5 Shock Wave Formation and Its Eventual Stalling 2.6 The Revival of the Shock Wave- the Neutrino Mechanism 2.7 Multi-Dimensional Hydrodynamic Simulations and the Present Scenario 2.8 The Supernova SN1987A 2.9 Detection of Neutrinos from Future Supernova Events References 3 Neutron Stars 3.1 History and Discovery of Neutron Stars 3.2 Observational Constraints on Neutron Stars 3.2.1 Mass 3.2.2 Radius 3.2.3 Moment of Inertia 3.3 Compositions and Novel Phases of Neutron Stars—Crust to Core 3.4 Equation of State Models of Neutron Star Matter 3.4.1 Microscopic Models 3.4.2 Chiral Effective Field Theory Models 3.4.3 Phenomenological Models 3.4.4 EoS Models of Matter at Sub-saturation Density 3.4.4.1 Baym–Pethick–Sutherland Model of Outer Crust 3.4.4.2 EoS Models of Inner Crust 3.4.4.3 Extended Nuclear Statistical Equilibrium Model 3.5 Relativistic Field Theoretical Models for Dense Matter at Zero and Finite Temperatures 3.5.1 Relativistic Mean Field Models 3.5.1.1 Hyperon-Hyperon Interaction 3.5.2 Bose–Einstein Condensates of (Anti)kaons 3.5.3 Quark Matter 3.5.3.1 Unpaired Quark Matter 3.5.3.2 Color Superconductivity in Quark Matter 3.5.3.3 Nambu-Jona-Lasinio Model for Quark Matter 3.5.4 Density Dependent Hadronic Field Theory at Finite Temperature 3.5.5 Antikaon Condensation at Finite Temperature 3.5.6 Nuclear Physics Constraints on EoS 3.6 Tolman–Oppenheimer–Volkoff Equation and Structures of Neutron Stars 3.7 Stable Branch of Compact Stars Beyond Neutron Star Branch 3.8 Rotating Neutron Stars, Moment of Inertia and Quadrupole Moment 3.8.1 Slowly Rotating Neutron Stars 3.8.2 Fully Relativistic, Nonlinear Models of Rapidly Rotating Neutron Stars 3.9 Neutron Star Matter in Strongly Quantizing Magnetic Fields 3.9.1 Magnetized Neutron Star Crusts 3.9.2 Dense Matter in Strong Magnetic Fields 3.10 EoS Tables for Supernova and Binary Neutron Star Merger Simulations Appendix 1 References 4 Binary Neutron Star Mergers 4.1 Gravitational Waves as New Window into Neutron Stars 4.2 First Binary Neutron Star Merger GW170817 and Multimessenger Astrophysics 4.3 Tidal Deformability, Love Number, and EoS 4.4 I-Love-Q Universal Relations 4.5 Inspiral Phase of BNS Merger, Tidal Deformability, and Cold EoS 4.6 Neutron Star Radius Determination from Tidal Deformability 4.7 Hot and Neutrino-Trapped Merger Remnants and Finite Temperature EoSs 4.7.1 Fate of BNS Merger Remnants 4.7.2 Upper Bound on Maximum Mass of Neutron Stars from GW170817 4.7.3 Finite Temperature EoSs and Imprints of Exotic Matter in GW Signals References 5 Synthesis of Heavy Elements in the Universe 5.1 Different Modes of Nucleosynthesis: The s-, the r-, and the p-Processes 5.1.1 The s-Process 5.1.2 The r-Process 5.1.3 The p-Process 5.2 Conditions for Production of Elements by the r-Process and the Sites 5.2.1 The Waiting-Point Nuclei 5.2.2 Fission Cycling 5.2.3 Freeze-Out 5.2.4 Conditions Needed for the r-Process 5.2.5 The Collapse of Massive Stars as Site for the r-Process 5.2.6 Neutron Star–Neutron Star/Black Hole Merger as Site for the r-Process 5.3 Inputs for Nuclear Modelling of the r-Process 5.3.1 Nuclear Masses/Binding Energies 5.3.2 Beta Decay Rates 5.3.3 Neutron Capture Rates 5.4 Electromagnetic Counterpart of GW170817 and Ejected Matter in BNS Merger 5.5 Decompression of Ejected Neutron-Rich Matter in Lattimer and Schramm Model 5.6 Kilonova Model 5.7 Heavy Element Synthesis in Neutron-Rich Matter Ejected in GW170817 References Index