Abstract
It is a long-standing intriguing problem to explore the synthesis of elements, and extensive studies are going on (See Clayton (Principles of Stellar Evolution and Nucleosynthesis, The University of Chicago Press, Chicago, 1968, [1]), Rolfs and Rodney (Cauldrons in the Cosmos, The University of Chicago Press, Chicago, 1988, [2]), Thompson and Nunes (Nuclear Reactions for Astrophysics: Principles, Calculation and Applications of Low-Energy Reactions, Cambridge University Press, Cambridge, 2009, [3]), VHS Element Genesis—Solving the Mystery, 2001, [4]). Roughly speaking, the synthesis of elements can be divided into the primordial nucleosynthesis, which is also called the Big Bang nucleosynthesis, and the stellar nucleosynthesis. The light elements such as deuterons , He and Li have been synthesized by nuclear reactions within 3–15 min after the Big Bang. This is the Big Bang nucleosynthesis. It terminates at the elements of mass number 7, since there is no stable nucleus of mass number 8. Stars started to be formed about one billion years later. Then, thermal nuclear reactions took place inside stars, and nuclei up to Fe, which has the largest binding energy per nucleon, have been successively synthesized depending on the mass of each star. (Precisely speaking, the nucleus which has the largest binding energy per nucleon is \({}^{62}_{28}\)Ni as remarked in Chap. 2.) Nuclei beyond Fe are synthesized either slowly by the neutron capture reactions called slow process (s-process) inside red giant stars, or synthesized by the explosive astrophysical phenomenon called rapid process (r-process). Nuclei with extremely large mass number such as U are thought to be synthesized at the supernovae explosion, which is one of the last stages of stars. In this chapter we learn some basics concerning the nuclear reactions related to nucleosynthesis (See Clayton (Principles of Stellar Evolution and Nucleosynthesis, 1968, [1]), Rolfs and Rodney (Cauldrons in the Cosmos, 1988, [2]), Thompson and Nunes (Nuclear Reactions for Astrophysics: Principles, Calculation and Applications of Low-Energy Reactions, Cambridge University Press, Cambridge, 2009, [3]) for details).
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Notes
- 1.
The actual reaction rate per pair is given by multiplying the pair density.
- 2.
Large neutron fluxes are expected in supernovae explosions. Consequently, neutron-rich nuclei are successively synthesized by (n,\(\gamma \)) reaction. The binding energy of neutron becomes small if the number of excess neutrons gets too large. The (n,\(\gamma \)) reaction then becomes balanced with the inverse (\(\gamma \),n) reaction, and the synthesis does not proceed further. Eventually, the unstable neutron-rich nucleus either proceeds towards stability line via \(\beta \)-decays, or repeats (n,\(\gamma \)) reactions after increasing the atomic number via \(\beta \)-decays to synthesize nuclei with still larger proton and neutron numbers. The r-process path is thus determined.
- 3.
The regions where the neutron number does not change for a while in the r-process nucleosynthesis are called waiting points and the corresponding nuclei are called waiting point nuclei. It is considered that the peaks on the left side in Fig. 1.7 appear reflecting the waiting points.
- 4.
Recent research on neutron stars suggests that the rp-process ends at \(^{105}_{~52}\)Te.
References
D.D. Clayton, Principles of Stellar Evolution and Nucleosynthesis (The University of Chicago Press, Chicago, 1968)
C.E. Rolfs, W.S. Rodney, Cauldrons in the Cosmos (The University of Chicago Press, Chicago, 1988)
I.J. Thompson, F.M. Nunes, Nuclear Reactions for Astrophysics: Principles, Calculation and Applications of Low-Energy Reactions (Cambridge University Press, Cambridge, 2009)
VHS Element Genesis—Solving the Mystery, Sci. Eds. Y. Motizuki, I. Tanihata, Y. Yano, R. Boyd (RIKEN & Image Science, Inc., 2001)
M. Junker et al., Phys. Rev. C 57, 2700 (1998)
M. Arnould, S. Goriely, K. Takahashi, Phys. Rep. 450, 97 (2007)
J.N. Bahcall, Neutrino Astrophysics (Cambridge University Press, Cambridge, 1989)
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Takigawa, N., Washiyama, K. (2017). Synthesis of Elements. In: Fundamentals of Nuclear Physics. Springer, Tokyo. https://doi.org/10.1007/978-4-431-55378-6_9
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