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

概要

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With an increase of temperature in a stellar core in which helium has been consumed completely, various thermonuclear reactions occur successively: C^<12>+C^<12> reactions occur at 6×10^<8^°>K, Ne^<20>(γ,α)O^<16> reactions occur at 1.0×10^<9^°>K and O^<16>+O^<16> reactions occur at 1.25×10^<9^°>K. These reactions are accompanied by production and absorption of protons and α-particles, and various elements are synthesized. In the cases of C^<12>+C^<12> and O^<16>+O^<16> 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 Mg^<24>, Mg^<25>, Si^<28>, P^<31>, etc., if carbon is abundant initially, and Si^<28>, P^<31>, S^<32>, etc., if oxygen is abundant. Reactions next arising are Mg^<25>(γ, n), P^<31>(γ, p), S^<32>(γ, p), S^<32>(γ, α), etc., at 1.5×10^<9^°>K. Further, Mg^<24> and Si^<28> are disintegrated at 2×10^<9^°>K and then thermal equilibrium will be established for the concentrations of the disintegration products.
理論物理学刊行会の論文
1963-01-25