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Supernovae, Neutron Star Physics and Nucleosynthesis 2022 ed. [Kõva köide]

  • Formaat: Hardback, 207 pages, kõrgus x laius: 235x155 mm, kaal: 512 g, 29 Illustrations, color; 12 Illustrations, black and white; XVII, 207 p. 41 illus., 29 illus. in color., 1 Hardback
  • Sari: Astronomy and Astrophysics Library
  • Ilmumisaeg: 29-Mar-2022
  • Kirjastus: Springer Nature Switzerland AG
  • ISBN-10: 3030951707
  • ISBN-13: 9783030951702
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  • Formaat: Hardback, 207 pages, kõrgus x laius: 235x155 mm, kaal: 512 g, 29 Illustrations, color; 12 Illustrations, black and white; XVII, 207 p. 41 illus., 29 illus. in color., 1 Hardback
  • Sari: Astronomy and Astrophysics Library
  • Ilmumisaeg: 29-Mar-2022
  • Kirjastus: Springer Nature Switzerland AG
  • ISBN-10: 3030951707
  • ISBN-13: 9783030951702
Teised raamatud teemal:
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.
1 Introduction
1(4)
2 Theory of Supernova Explosions
5(44)
2.1 Overview: Historical
6(1)
2.2 Supernova Type la
7(1)
2.3 Gravitational Collapse and Pre-supernova Conditions
8(5)
2.4 Production of Neutrinos and Their Emission
13(5)
2.5 Shock Wave Formation and Its Eventual Stalling
18(4)
2.6 The Revival of the Shock Wave- the Neutrino Mechanism
22(8)
2.7 Multi-Dimensional Hydrodynamic Simulations and the Present Scenario
30(3)
2.8 The Supernova SN1987A
33(5)
2.9 Detection of Neutrinos from Future Supernova Events
38(11)
References
44(5)
3 Neutron Stars
49(86)
3.1 History and Discovery of Neutron Stars
49(2)
3.2 Observational Constraints on Neutron Stars
51(5)
3.2.1 Mass
51(1)
3.2.2 Radius
52(2)
3.2.3 Moment of Inertia
54(2)
3.3 Compositions and Novel Phases of Neutron Stars--Crust to Core
56(1)
3.4 Equation of State Models of Neutron Star Matter
57(12)
3.4.1 Microscopic Models
58(1)
3.4.2 Chiral Effective Field Theory Modelse
59(1)
3.4.3 Phenomenological Models
60(1)
3.4.4 EoS Models of Matter at Sub-saturation Density
61(8)
3.5 Relativistic Field Theoretical Models for Dense Matter at Zero and Finite Temperatures
69(24)
3.5.1 Relativistic Mean Field Models
70(5)
3.5.2 Bose-Einstein Condensates of (Anti)kaons
75(4)
3.5.3 Quark Matter
79(5)
3.5.4 Density Dependent Hadronic Field Theory at Finite Temperature
84(4)
3.5.5 Antikaon Condensation at Finite Temperature
88(2)
3.5.6 Nuclear Physics Constraints on EoS
90(3)
3.6 Tolman-Oppenheimer-olkoff Equation and Structures of Neutron Stars
93(2)
3.7 Stable Branch of Compact Stars Beyond Neutron Star Branch
95(3)
3.8 Rotating Neutron Stars, Moment of Inertia and Quadrupole Moment
98(8)
3.8.1 Slowly Rotating Neutron Stars
99(3)
3.8.2 Fully Relativistic, Nonlinear Models of Rapidly Rotating Neutron Stars
102(4)
3.9 Neutron Star Matter in Strongly Quantizing Magnetic Fields
106(8)
3.9.1 Magnetized Neutron Star Crusts
107(3)
3.9.2 Dense Matter in Strong Magnetic Fields
110(4)
3.10 EoS Tables for Supernova and Binary Neutron Star Merger Simulations
114(21)
References
122(13)
4 Binary Neutron Star Mergers
135(34)
4.1 Gravitational Waves as New Window into Neutron Stars
135(2)
4.2 First Binary Neutron Star Merger GW170817 and Multimessenger Astrophysics
137(1)
4.3 Tidal Deformability, Love Number, and EoS
138(5)
4.4 I-Love-Q Universal Relations
143(3)
4.5 Inspiral Phase of BNS Merger, Tidal Deformability, and Cold EoS
146(4)
4.6 Neutron Star Radius Determination from Tidal Deformability
150(6)
4.7 Hot and Neutrino-Trapped Merger Remnants and Finite Temperature EoSs
156(13)
4.7.1 Fate of BNS Merger Remnants
156(1)
4.7.2 Upper Bound on Maximum Mass of Neutron Stars from GW170817
157(3)
4.7.3 Finite Temperature EoSs and Imprints of Exotic Matter in GW Signals
160(2)
References
162(7)
5 Synthesis of Heavy Elements in the Universe
169(34)
5.1 Different Modes of Nucleosynthesis: The s-, the r-, and the p-Processes
169(11)
5.1.1 Thes-Process
173(5)
5.1.2 Ther-Process
178(2)
5.1.3 Thep-Process
180(1)
5.2 Conditions for Production of Elements by the r-Process and the Sites
180(7)
5.2.1 The Waiting-Point Nuclei
180(1)
5.2.2 Fission Cycling
181(1)
5.2.3 Freeze-Out
182(1)
5.2.4 Conditions Needed for the r-Process
182(2)
5.2.5 The Collapse of Massive Stars as Site for the r-Process
184(2)
5.2.6 Neutron Star-Neutron Star/Black Hole Merger as Site for the r-Process
186(1)
5.3 Inputs for Nuclear Modelling of the r-Process
187(4)
5.3.1 Nuclear Masses/Binding Energies
187(1)
5.3.2 Beta Decay Rates
188(2)
5.3.3 Neutron Capture Rates
190(1)
5.4 Electromagnetic Counterpart of GW170817 and Ejected Matter in BNS Merger
191(1)
5.5 Decompression of Ejected Neutron-Rich Matter in Lattimer and Schramm Model
192(3)
5.6 Kilonova Model
195(2)
5.7 Heavy Element Synthesis in Neutron-Rich Matter Ejected in GW170817
197(6)
References
198(5)
Index 203
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.