Supernovae, neutron star physics and nucleosynthesis
著者
書誌事項
Supernovae, neutron star physics and nucleosynthesis
(Astronomy and astrophysics library)
Springer, 2022
大学図書館所蔵 全6件
  青森
  岩手
  宮城
  秋田
  山形
  福島
  茨城
  栃木
  群馬
  埼玉
  千葉
  東京
  神奈川
  新潟
  富山
  石川
  福井
  山梨
  長野
  岐阜
  静岡
  愛知
  三重
  滋賀
  京都
  大阪
  兵庫
  奈良
  和歌山
  鳥取
  島根
  岡山
  広島
  山口
  徳島
  香川
  愛媛
  高知
  福岡
  佐賀
  長崎
  熊本
  大分
  宮崎
  鹿児島
  沖縄
  韓国
  中国
  タイ
  イギリス
  ドイツ
  スイス
  フランス
  ベルギー
  オランダ
  スウェーデン
  ノルウェー
  アメリカ
注記
Includes bibliographical references and index
内容説明・目次
内容説明
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.
目次
PREFACE1. 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)
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