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Prog. Theor. Phys. Vol. 29 No. 1 (1963) pp. 29-43

[ Full Text PDF : FREE ACCESS (1032K) ]

Thermonuclear Reactions in Stars Involving Heavy Ions up to the Formation of Iron Nuclei

Hiroshi Tsuda

Department of Nuclear Science, Kyoto University, Kyoto

(Received August 17, 1962)

Abstract:

With an increase of temperature in a stellar core in which helium has been consumed completely, various thermonuclear reactions occur successively: C12 + C12 reactions occur at 6 × 108 °K, Ne20 (γ , α)O16 reactions occur at 1.0 × 109 °K and O16 + O16 reactions occur at 1.25×109 °K. These reactions are accompanied by production and absorption of protons and α-particles, and various elements are synthesized. In the cases of C12 + C12 and O16 + O16 reactions, neutrons are also produced. If the stellar core is rich in carbon after helium burning, a considerable amount of heavy metals are produced, but if the core is rich in oxygen, heavy metals are scarecely produced. The elements remaining after oxygen burning are Mg24, Mg25, Si28, P31, etc., if carbon is abundant initially, and Si28, S32, etc., if oxygen is abundant. Reactions next arising are Mg25 (γ, n), P31(γ, p), S32(γ, p), S32(γ, α), etc., at 1.5 × 109 °K. Further, Mg24 and Si28 are disintegrated at 2 × 109 °K and then thermal equilibrium will be established for the concentrations of the disintegration products.


URL : http://ptp.ipap.jp/link?PTP/29/29/
DOI : 10.1143/PTP.29.29

[ Full Text PDF : FREE ACCESS (1032K) ] Citation:

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Citing Article(s) :

  1. Progress of Theoretical Physics Vol. 31 No. 4 (1964) pp. 727-729 :
    Neutrino Pair Emission from Excited Nuclei
    Shirô Sakashita and Minoru Nishida
  2. Progress of Theoretical Physics Vol. 34 No. 1 (1965) pp. 188-189 :
    Neutrino Pair Emission From Excited Nuclei. II
    Minoru Nishida and Shiro Sakashita
  3. Progress of Theoretical Physics Vol. 39 No. 6 (1968) pp. 1432-1447 :
    Evolution of Carbon Stars. II
    Daiichiro Sugimoto, Yoshiaki Yamamoto, Reiun Hōshi and Chushiro Hayashi

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