Supernovae and Nucleosynthesis : : An Investigation of the History of Matter, from the Big Bang to the Present / / David Arnett.
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...
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| Superior document: | Title is part of eBook package: De Gruyter Princeton University Press eBook-Package Archive 1927-1999 |
|---|---|
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| Place / Publishing House: | Princeton, NJ : : Princeton University Press, , [2020] ©1996 |
| Year of Publication: | 2020 |
| Language: | English |
| Series: | Princeton Series in Astrophysics ;
55 |
| Online Access: | |
| Physical Description: | 1 online resource (496 p.) :; 67 tables, 119 line drawings |
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| LEADER | 08785nam a22012495i 4500 | ||
|---|---|---|---|
| 001 | 9780691221663 | ||
| 003 | DE-B1597 | ||
| 005 | 20210830012106.0 | ||
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| 007 | cr || |||||||| | ||
| 008 | 210830t20201996nju fo d z eng d | ||
| 020 | |a 9780691221663 | ||
| 024 | 7 | |a 10.1515/9780691221663 |2 doi | |
| 035 | |a (DE-B1597)572666 | ||
| 035 | |a (OCoLC)1206239361 | ||
| 040 | |a DE-B1597 |b eng |c DE-B1597 |e rda | ||
| 041 | 0 | |a eng | |
| 044 | |a nju |c US-NJ | ||
| 072 | 7 | |a SCI005000 |2 bisacsh | |
| 100 | 1 | |a Arnett, David, |e author. |4 aut |4 http://id.loc.gov/vocabulary/relators/aut | |
| 245 | 1 | 0 | |a Supernovae and Nucleosynthesis : |b An Investigation of the History of Matter, from the Big Bang to the Present / |c David Arnett. |
| 264 | 1 | |a Princeton, NJ : |b Princeton University Press, |c [2020] | |
| 264 | 4 | |c ©1996 | |
| 300 | |a 1 online resource (496 p.) : |b 67 tables, 119 line drawings | ||
| 336 | |a text |b txt |2 rdacontent | ||
| 337 | |a computer |b c |2 rdamedia | ||
| 338 | |a online resource |b cr |2 rdacarrier | ||
| 347 | |a text file |b PDF |2 rda | ||
| 490 | 0 | |a Princeton Series in Astrophysics ; |v 55 | |
| 505 | 0 | 0 | |t Frontmatter -- |t Contents -- |t List of Figures -- |t List of Tables -- |t Preface -- |t 1 Introduction -- |t 2 Abundances of Nuclei -- |t Introduction -- |t 2.1 What Are Abundances? -- |t 2.2 Solar System Abundances -- |t 2.3 Stellar Atmospheres -- |t 2.4 Meteorites -- |t 2.5 Cosmic Rays -- |t 2.6 Other Aspects -- |t 3 Some Aspects of Nuclear Physics -- |t Introduction -- |t 3.1 Nuclear Masses -- |t 3.2 Nuclear Stability -- |t 3.3 Coulomb Barrier -- |t 3.4 Resonances -- |t 3.5 Reverse Rates -- |t 3.6 Heavy-Ion Reactions -- |t 3.7 Weak Interactions in Nuclei -- |t 3.8 Sources of Rates -- |t 4 Nuclear Reaction Networks -- |t Introduction -- |t 4.1 Network Equations -- |t 4.2 Solutions: Steady State -- |t 4.3 Solutions: Equilibria -- |t 4.4 Solutions: General Method -- |t 4.5 Energy Generation -- |t 4.6 Mixing and Hydrodynamics -- |t 4.7 Freezeout -- |t 5 Cosmological Nucleosynthesis -- |t Introduction -- |t 5.1 Kinematics -- |t 5.2 Radiation and Particles -- |t 5.3 Weak Interaction Freezeout -- |t 5.4 Cosmological Nucleosynthesis -- |t 5.5 Further Implications -- |t 6 Some Properties of Stars -- |t Introduction -- |t 6.1 Stellar Evolution Equations -- |t 6.2 Standard Model -- |t 6.3 Nuclear Energy -- |t 6.4 Neutrino Processes -- |t 6.5 Stellar Energy -- |t 6.6 Ignition Masses -- |t 6.7 Final States -- |t 7 Hydrogen-Burning Stars -- |t Introduction -- |t 7.1 Birth of Stars -- |t 7.2 Burning Processes -- |t 7.3 Main Sequence -- |t 7.4 Convective Cores -- |t 7.5 Shell Burning -- |t 7.6 Nucleosynthesis -- |t 8 Helium-Burning Stars -- |t Introduction -- |t 8.1 Thermonuclear Features -- |t 8.2 Ignition -- |t 8.3 Core Nucleosynthesis -- |t 8.4 Shell Nucleosynthesis -- |t 8.5 M-Ma Relation -- |t 8.6 Implications -- |t 9 Explosive Nucleosynthesis -- |t Introduction -- |t 9.1 Parameters -- |t 9.2 Carbon and Neon -- |t 9.3 Oxygen -- |t 9.4 Silicon and e-Process -- |t 9.5 Neutron Excess and Galactic Evolution -- |t 9.6 Yield Puzzle -- |t 10 Neutrino-Cooled Stars -- |t Introduction -- |t 10.1 Neutrinos and Convection -- |t 10.2 Core Evolution -- |t 10.3 Stellar Structure -- |t 10.4 Shell Nucleosynthesis -- |t 11 Thermonuclear Explosions -- |t Introduction -- |t 11.1 Thermonuclear Flames -- |t 11.2 Degenerate Instability -- |t 11.3 Convection and Urea -- |t 11.4 Yields from Degenerate Instability -- |t 11.5 He Detonation -- |t 11.6 Pair Instability -- |t 11.7 Oxygen Burning and Beyond -- |t 12 Gravitational Collapse -- |t Introduction -- |t 12.1 Historical Overview -- |t 12.2 Neutronization and Dissociation -- |t 12.3 Neutrino Trapping -- |t 12.4 Collapse -- |t 12.5 Bounce -- |t 12.6 Ejection of Matter -- |t 13 Supernovae -- |t Introduction -- |t 13.1 An Overview -- |t 13.2 Shock Emergence -- |t 13.3 Expansion and Radiative Diffusion -- |t 13.4 Radioactive Heating -- |t 13.5 Recombination -- |t 13.6 SN1987A -- |t 13.7 Type II Supernovae and SN1993J -- |t 13.8 Type I Supernovae -- |t 14 Galactic Evolution -- |t Introduction -- |t 14.1 Galactic Evolution Equations -- |t 14.2 Initial Mass Functions -- |t 14.3 One-Zone Models -- |t 14.4 Absolute Yields -- |t 14.5 The Galactic Disk -- |t 14.6 Primordial Stellar Yields -- |t 14.7 Critical Uncertainties -- |t Appendixes -- |t A. Solar System Abundances -- |t B. Equations of State -- |t C. Stellar Structure -- |t D. Supernova Light Curves -- |t References -- |t Index -- |t About the Author |
| 506 | 0 | |a restricted access |u http://purl.org/coar/access_right/c_16ec |f online access with authorization |2 star | |
| 520 | |a 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 thermonuclear reactors, otherwise known as stars. Our current understanding is presented systematically and quantitatively, by combining simple analytic models with new state-of-the-art computer simulations. The narrative begins with the clues (primarily the solar system abundance pattern), the constraining physics (primarily nuclear and particle physics), and the thermonuclear burning in the Big Bang itself. It continues with a step-by-step description of how stars evolve by nuclear reactions, a critical investigation of supernova explosion mechanisms and the formation of neutron stars and of black holes, and an analysis of how such explosions appear to astronomers (illustrated by comparison with recent observations). It concludes with a synthesis of these ideas for galactic evolution, with implications for nucleosynthesis in the first generation of stars and for the solar system abundance pattern. Emphasis is given to questions that remain open, and to active research areas that bridge the disciplines of astronomy, cosmochemistry, physics, and planetary and space science. Extensive references are given. | ||
| 538 | |a Mode of access: Internet via World Wide Web. | ||
| 546 | |a In English. | ||
| 588 | 0 | |a Description based on online resource; title from PDF title page (publisher's Web site, viewed 30. Aug 2021) | |
| 650 | 7 | |a SCIENCE / Physics / Astrophysics. |2 bisacsh | |
| 653 | |a Chandrasekhar mass. | ||
| 653 | |a Fermi selection rules. | ||
| 653 | |a Galactic disk. | ||
| 653 | |a Kepler. | ||
| 653 | |a Lagrangian coordinates. | ||
| 653 | |a Ledoux criterion. | ||
| 653 | |a O shell burning. | ||
| 653 | |a absorption lines. | ||
| 653 | |a accretion. | ||
| 653 | |a alpha decay. | ||
| 653 | |a angular momentum. | ||
| 653 | |a backward differencing. | ||
| 653 | |a baryogenesis. | ||
| 653 | |a burning stages. | ||
| 653 | |a chaos. | ||
| 653 | |a coulomb repulsion. | ||
| 653 | |a curve of growth. | ||
| 653 | |a decoupling. | ||
| 653 | |a deflagration. | ||
| 653 | |a deuterium. | ||
| 653 | |a energy generation rate. | ||
| 653 | |a expansional cooling. | ||
| 653 | |a explosive time-scale. | ||
| 653 | |a freezeout. | ||
| 653 | |a gamma emission. | ||
| 653 | |a gravitational contraction. | ||
| 653 | |a helium burning. | ||
| 653 | |a hydrodynamics. | ||
| 653 | |a hydrogen burning. | ||
| 653 | |a ignition mass. | ||
| 653 | |a implicit differencing. | ||
| 653 | |a ionization. | ||
| 653 | |a lepton number. | ||
| 653 | |a magic numbers. | ||
| 653 | |a mass-luminosity relation. | ||
| 653 | |a mixing-length theory. | ||
| 653 | |a molecular clouds. | ||
| 653 | |a neutral currents. | ||
| 653 | |a numerical instability. | ||
| 653 | |a overproduction. | ||
| 653 | |a pairing energy. | ||
| 653 | |a photoelectric effect. | ||
| 653 | |a quartic. | ||
| 653 | |a radiation entropy. | ||
| 653 | |a radiation pressure. | ||
| 653 | |a shock emergence. | ||
| 653 | |a solar neighborhood. | ||
| 653 | |a spectral types. | ||
| 653 | |a stiff equations. | ||
| 653 | |a turbulent pressure. | ||
| 653 | |a uniform approximation. | ||
| 653 | |a valley of stability. | ||
| 773 | 0 | 8 | |i Title is part of eBook package: |d De Gruyter |t Princeton University Press eBook-Package Archive 1927-1999 |z 9783110442496 |
| 856 | 4 | 0 | |u https://doi.org/10.1515/9780691221663?locatt=mode:legacy |
| 856 | 4 | 0 | |u https://www.degruyter.com/isbn/9780691221663 |
| 856 | 4 | 2 | |3 Cover |u https://www.degruyter.com/cover/covers/9780691221663.jpg |
| 912 | |a 978-3-11-044249-6 Princeton University Press eBook-Package Archive 1927-1999 |c 1927 |d 1999 | ||
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