Nuclear Physics of Stars
John Wiley & Sons, 09.04.2007 - 666 Seiten
Thermonuclear reactions in stars is a major topic in the field of nuclear astrophysics, and deals with the topics of how precisely stars generate their energy through nuclear reactions, and how these nuclear reactions create the elements the stars, planets and - ultimately - we humans consist of. The present book treats these topics in detail. It also presents the nuclear reaction and structure theory, thermonuclear reaction rate formalism and stellar nucleosynthesis. The topics are discussed in a coherent way, enabling the reader to grasp their interconnections intuitively. The book serves both as a textbook, with many examples and end-of-chapter exercises, but also as a reference book for use by researchers working in the field of nuclear astrophysics.
Was andere dazu sagen - Rezension schreiben
Es wurden keine Rezensionen gefunden.
Nuclear Physics of Stars Christian Iliadis
Nuclear Physics Experiments
Nuclear Burning Stages and Processes
A Solutions of the Schrodinger Equation in Three Dimensions
B Quantum Mechanical Selection Rules
Andere Ausgaben - Alle anzeigen
3-decay a-particles abundance flow amount angular correlation angular momentum astrophysical atomic beam branching ratio capture reaction center-of-mass chain channel charged-particle CNO cycles CNO1 core corresponding Coulomb barrier cross section decay constant depends detector displayed in Fig efficiency elastic scattering electron emission emitted energy generation rate equilibrium evolution example excited factor Gamow peak given half-lives helium burning hydrogen burning incident initial interaction isotopes located mass fraction mass number mean lifetime measured narrow resonance network calculation neutrino neutron capture nonresonant nuclear reaction nuclei nucleon nucleosynthesis nuclides obtained parity partial widths particles photodisintegration potential produced projectile proton pulse height Q-value quantity r-process radiation radioactive reaction rates result S-factor s-wave seed nuclei shell shown in Fig silicon solar system solid line spectrum spin stellar plasma stopping power supernovae target nuclei temperature and density thermal tion total number values versus waiting point wave function yield curve