Nuclear Physics of StarsJohn Wiley & Sons, 19.03.2015 - 672 Seiten Most elements are synthesized, or "cooked", by thermonuclear reactions in stars. The newly formed elements are released into the interstellar medium during a star's lifetime, and are subsequently incorporated into a new generation of stars, into the planets that form around the stars, and into the life forms that originate on the planets. Moreover, the energy we depend on for life originates from nuclear reactions that occur at the center of the Sun. Synthesis of the elements and nuclear energy production in stars are the topics of nuclear astrophysics, which is the subject of this book. It presents nuclear structure and reactions, thermonuclear reaction rates, experimental nuclear methods, and nucleosynthesis in detail. These topics are discussed in a coherent way, enabling the reader to grasp their interconnections intuitively. The book serves both as a textbook for advanced undergraduate and graduate students, with worked examples and end-of-chapter excercises, but also as a reference book for use by researchers working in the field of nuclear astrophysics. |
Inhalt
| 1 | |
Chapter 2 Nuclear Reactions | 73 |
Chapter 3 Thermonuclear Reactions | 139 |
Chapter 4 Nuclear Physics Experiments | 207 |
Chapter 5 Nuclear Burning Stages and Processes | 349 |
Appendix A Solutions of the Schrödinger
Equation in Three Dimensions | 569 |
Appendix B Quantum Mechanical Selection Rules | 573 |
Appendix C Kinematics | 579 |
Appendix D Angular Correlations | 587 |
Color Plates | 613 |
| 627 | |
| 639 | |
EULA | 654 |
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Häufige Begriffe und Wortgruppen
abundance flow angular correlation angular momentum astrophysical atomic beam branching ratio charged-particle CNO cycles CNO1 core corresponding Coulomb barrier cross section decay constant depends detector elastic scattering electron capture emission emitted energy generation rate evolution example excited explosive E𝛾 factor Gamow peak given helium burning hydrogen burning incident initial interaction isotopic located mass fraction mass number Maxwell–Boltzmann distribution mean lifetime measured narrow resonance network calculation neutrino neutron excess nuclear reactions nuclei nucleon nucleosynthesis nuclides number density observed obtained p-nuclides partial widths particles photodisintegration potential processes produced projectile proton pulse height Q-value quantity r-process radiation radioactive reaction rates respectively result S-factor seed nuclei shell shown in Figure silicon burning solar system solid line species spin stopping power target nuclei temperature and density thermal thermonuclear thickness tion total number transition type Ia supernovae values versus waiting point wave function white dwarf 𝜂 𝜃 𝜌