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 theejected material from GW170817. This monograph is written for graduate students and researchers in the field of nuclear astrophysics.

Autorentext

Debades Bandyopadhyay is a former senior professor at the Astroparticle and Cosmology Division, Saha Institute of Nuclear Physics, Kolkata, India. He obtained his PhD degree from the University of Calcutta. He worked as a postdoctoral researcher at the Institute for Theoretical Physics, Frankfurt University, Germany. His areas of research include topics ranging from nuclei to neutron stars, and he is particularly involved in the study of dense matter in neutron star interiors. He was the recipient of the Alexander von Humboldt Fellowship, Germany. He is a regular visitor to the Frankfurt University and Frankfurt Institute for Advanced Studies (FIAS), Germany.

Kamales Kar is presently a visiting professor at the Ramakrishna Mission Vivekananda Educational and Research Institute, Belur Math, West Bengal, India. He retired from the Theory Division of Saha Institute of Nuclear Physics as a senior professor. He received his PhD degree from the University of Rochester, USA, working on problems related to nuclear structure. After postdoctoral positions at the University of Toronto, Canada, and Physical Research Laboratory, Ahmedabad, India, he joined the faculty of Saha Institute. He was a regular visitor to the University of Padova, Italy, and Complutense University of Madrid, Spain, for research collaborations. His research interests are in neutrino physics and astrophysics as well as in areas of nuclear astrophysics and nuclear structure.

Inhalt
PREFACE

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

3. NEUTRON STARS

3.1 History and discovery of neutron stars

3.2 Observational Constraints on neutron stars

3.3 Compositions and novel phases of neutron stars - crust to core

3.4 Equation of State (EoS) models of neutron star matter

3.5 Relativistic field theoretical models for dense matter at zero and finite temperatures

3.6 Tolman-Oppenheimer-Volkoff Equation and Structures of neutron stars

3.7 A stable branch of compact stars beyond neutron star

3.8 Rotating neutron stars, moment of inertia (I) and quadrupole moment (Q)

3.9 Neutron star matter in strongly quantizing magnetic fields

3.10 EoS tables for supernova and binary neutron star merger simulations

4. BINARY NEUTRON STAR MERGERS

4.1 Gravitational waves as new window into neutron stars

4.2 First binary neutron star (BNS) merger GW170817 and multi-messenger astrophysics

4.3 Tidal deformability, LOVE number and EoS 4.4 I-Love-Q universal relations

4.5 Late 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 remnant and finite temperature EoS

5. SYNTHESIS OF HEAVY ELEMENTS IN THE UNIVERSE

5.1 s-, r- and p-processes

5.2 Conditions for production of elements by r- process and the sites

5.3 Electromagnetic counterpart of GW170817 and ejected matter in BNS merger

5.4 Decompression of ejected neutron rich matter in Lattimer and Schramm model

5.5 Kilonova model

5.6 Heavy element synthesis in neutron rich matter ejected in GW170817

INDEX BIBLIOGRAPHY (eventually at chapter-ends)