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Nucleosynthesis basics and applications to supernovae
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- By F.-K. Thielemann, Departement für Physik und Astronomie, Universität Basel, CH–4056 Basel, Switzerland, institute for Theoretical Physics, University of California, Santa Barbara, CA 93106–4030, T. Rauscher, Departement für Physik und Astronomie, Universität Basel, CH–4056 Basel, Switzerland, C. Freiburghaus, Departement für Physik und Astronomie, Universität Basel, CH–4056 Basel, Switzerland, institute for Theoretical Physics, University of California, Santa Barbara, CA 93106–4030, K. Nomoto, Department of Astronomy and Research Center for the Early Universe, University of Tokyo, Tokyo 113, Japan, institute for Theoretical Physics, University of California, Santa Barbara, CA 93106–4030, M. Hashimoto, Department of Physics, Faculty of Science, Kyushu University, Pukuoka 810, Japan, B. Pfeiffer, Institut für Kernchemie, Universität Mainz, D–55128 Mainz, Germany, K.-L. Kratz, Institut für Kernchemie, Universität Mainz, D–55128 Mainz, Germany
- Edited by Jorge G. Hirsch, Center of Research and Advanced Studies, National Polytechnic Institute, Mexico City, Danny Page, Universidad Nacional Autónoma de México
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- Book:
- Nuclear and Particle Astrophysics
- Published online:
- 07 September 2010
- Print publication:
- 13 August 1998, pp 27-78
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- Chapter
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Summary
This review concentrates on nucleosynthesis processes in general and their applications to massive stars and supernovae. A brief initial introduction is given to the physics in astrophysical plasmas which governs composition changes. We present the basic equations for thermonuclear reaction rates and nuclear reaction networks. The required nuclear physics input for reaction rates is discussed, i.e. cross sections for nuclear reactions, photodisintegrations, electron and positron captures, neutrino captures, inelastic neutrino scattering, and beta–decay half–lives. We examine especially the present state of uncertainties in predicting thermonuclear reaction rates, while the status of experiments is discussed by others in this volume (see M. Wiescher). It follows a brief review of hydrostatic burning stages in stellar evolution before discussing the fate of massive stars, i.e. the nucleosynthesis in type II supernova explosions (SNe II). Except for SNe la, which are explained by exploding white dwarfs in binary stellar systems (which will not be discussed here), all other supernova types seem to be linked to the gravitational collapse of massive stars (M>8M⊙) at the end of their hydrostatic evolution. SN1987A, the first type II supernova for which the progenitor star was known, is used as an example for nucleosynthesis calculations. Finally, we discuss the production of heavy elements in the r–process up to Th and U and its possible connection to supernovae.